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[[File:Starsinthesky.jpg|right|300px|thumb|A [[stellar nursery|star-forming]] region in the [[Large Magellanic Cloud]]. [[NASA]]/[[ESA]] image]]
[[File:The Sun by the Atmospheric Imaging Assembly of NASA's Solar Dynamics Observatory - 20100819.jpg|right|300px|thumb|False-color imagery of the [[Sun]], a [[G-type main-sequence star]], the closest to Earth.]]
A '''star''' is a [[Stellar mass|massive]], luminous sphere of [[plasma (physics)|plasma]] held together by its own [[gravity]]. The nearest star to [[Earth]] is the [[Sun]], which is the source of most of the planet's energy. Some other stars are visible from Earth during the night, appearing as a multitude of fixed luminous points due to their immense distance. Historically, the most prominent stars were grouped into [[constellation]]s and [[Asterism (astronomy)|asterisms]], and the brightest stars gained proper names. Extensive [[star catalogue|catalogues of stars]] have been assembled by astronomers, which provide standardized [[star designation]]s.
 
For at least a portion of its life, a star shines due to [[thermonuclear fusion]] of [[hydrogen]] into [[helium]] in its core, releasing energy that traverses the star's interior and then [[radiation|radiates]] into [[outer space]]. Once the hydrogen in the core of a star is nearly exhausted, almost all naturally occurring elements heavier than helium are created by [[stellar nucleosynthesis]] during the star's lifetime and, for some stars, by [[supernova nucleosynthesis]] when it explodes. Near the end of its life, a star can also contain [[degenerate matter]]. [[Astronomer]]s can determine the [[mass]], age, [[metallicity]] (chemical composition), and many other properties of a star by observing its motion through space, [[luminosity]], and [[Astronomical spectroscopy|spectrum]] respectively. The total mass of a star is the principal determinant of its [[stellar evolution|evolution]] and eventual fate. Other characteristics of a star, including diameter and temperature, change over its life, while the star's environment affects its rotation and movement. A plot of the temperature of many stars against their luminosities, known as a [[Hertzsprung–Russell diagram]] (H–R diagram), allows the age and evolutionary state of a star to be determined.
 
A star's life [[star formation|begins]] with the gravitational collapse of a gaseous [[nebula]] of material composed primarily of hydrogen, along with helium and trace amounts of heavier elements. Once the stellar core is sufficiently dense, hydrogen becomes steadily converted into helium through nuclear fusion, releasing energy in the process.<ref name="sunshine">{{cite web
| last = Bahcall | first = John N.
| date = June 29, 2000
| url = http://nobelprize.org/nobel_prizes/physics/articles/fusion/index.html
| title = How the Sun Shines | publisher = Nobel Foundation
| accessdate = 2006-08-30 }}</ref> The remainder of the star's interior carries energy away from the core through a combination of [[radiation|radiative]] and [[convection|convective]] processes. The star's internal pressure prevents it from collapsing further under its own gravity. Once the hydrogen [[fuel]] at the core is exhausted, a star with at least 0.4 times the mass of the Sun<ref name="late stages">{{cite web
| last = Richmond | first = Michael
| url = http://spiff.rit.edu/classes/phys230/lectures/planneb/planneb.html
| title = Late stages of evolution for low-mass stars
| publisher = Rochester Institute of Technology
| accessdate = 2006-08-04 }}</ref> expands to become a [[red giant]], in some cases fusing heavier [[chemical element|elements]] at the core or in shells around the core. The star then evolves into a degenerate form, recycling a portion of its matter into the interstellar environment, where it will contribute to the formation of a new generation of stars with a higher proportion of heavy elements.<ref>{{cite web
| url = http://observe.arc.nasa.gov/nasa/space/stellardeath/stellardeath_intro.html
| archiveurl = http://web.archive.org/web/20080210154901/http://observe.arc.nasa.gov/nasa/space/stellardeath/stellardeath_intro.html
| archivedate = 2008-02-10
| title = Stellar Evolution & Death
| publisher = NASA Observatorium
| accessdate = 2006-06-08 }}</ref> Meanwhile, the core becomes a [[stellar remnant]]: a [[white dwarf]], a [[neutron star]], or (if it is sufficiently massive) a [[black hole]].
 
[[Binary star|Binary]] and multi-star systems consist of two or more stars that are gravitationally bound, and generally move around each other in stable [[orbit]]s. When two such stars have a relatively close orbit, their gravitational interaction can have a significant impact on their evolution.<ref name="iben">{{cite journal
| last = Iben | first = Icko, Jr.
| title=Single and binary star evolution
| journal=Astrophysical Journal Supplement Series
| year=1991 | volume=76 | pages=55–114
| bibcode=1991ApJS...76...55I
| doi=10.1086/191565 }}</ref> Stars can form part of a much larger gravitationally bound structure, such as a [[star cluster]] or a [[galaxy]].
 
==Observation history==
[[File:Dibuix de Leo.png|thumb|220px|right|People have seen patterns in the stars since ancient times.<ref name="forbes" /> This 1690 depiction of the constellation of [[Leo (constellation)|Leo]], the lion, is by [[Johannes Hevelius]].<ref>{{cite book
| first=Johannis | last=Hevelius | year=1690
| title=Firmamentum Sobiescianum, sive Uranographia
| location=Gdansk }}</ref>]]
[[File:LeoCC.jpg|220px|thumbnail|right|The constellation of [[Leo (constellation)|Leo]] as it can be seen by the naked eye. Lines have been added.]]
Historically, stars have been important to [[civilization]]s throughout the world. They have been part of [[religious]] practices and used for [[celestial navigation]] and orientation. Many ancient astronomers believed that stars were permanently affixed to a [[heavenly sphere]], and that they were immutable. By convention, astronomers grouped stars into [[constellation]]s and used them to track the motions of the [[planets]] and the inferred position of the Sun.<ref name="forbes">{{cite book
| last1=Forbes | first1=George | title=History of Astronomy
| publisher=Watts & Co. | location=London | year=1909
| url=http://www.gutenberg.org/ebooks/8172
| isbn=1-153-62774-4 }}</ref> The motion of the Sun against the background stars (and the horizon) was used to create [[Solar calendar|calendars]], which could be used to regulate agricultural practices.<ref>{{cite web
| last=Tøndering | first=Claus
| url=http://webexhibits.org/calendars/calendar-ancient.html
| title=Other ancient calendars | publisher=WebExhibits
| accessdate=2006-12-10 }}</ref> The [[Gregorian calendar]], currently used nearly everywhere in the world, is a [[solar calendar]] based on the angle of the Earth's rotational axis relative to its local star, the Sun.
 
The oldest accurately dated [[star chart]] appeared in ancient [[Egyptian astronomy]] in 1534 BC.<ref>{{cite journal
| last=von Spaeth | first=Ove
| title=Dating the Oldest Egyptian Star Map
| journal=Centaurus International Magazine of the History of Mathematics, Science and Technology
| year=2000 | volume=42 | issue=3 | pages=159–179
| url=http://www.moses-egypt.net/star-map/senmut1-mapdate_en.asp
| accessdate=2007-10-21 }}</ref> The [[Babylonian star catalogues|earliest known star catalogues]] were compiled by the ancient [[Babylonian astronomy|Babylonian astronomers]] of [[Mesopotamia]] in the late 2nd millennium BC, during the [[Kassites|Kassite Period]] (''ca.'' 1531–1155 BC).<ref name="north 1995 30 31">{{cite book
| last=North | first=John | year=1995
| title=The Norton History of Astronomy and Cosmology
| location=New York and London | pages=30–31
| publisher=W.W. Norton & Company | isbn=0-393-03656-1 }}</ref>
 
The first [[star catalogue]] in [[Greek astronomy]] was created by [[Aristillus]] in approximately 300 BC, with the help of [[Timocharis]].<ref>{{cite book
| last=Murdin | first=P. |date=November 2000
| chapter=Aristillus (c. 200 BC)
| doi=10.1888/0333750888/3440
| title=Encyclopedia of Astronomy and Astrophysics
| bibcode=2000eaa..bookE3440
| isbn=0-333-75088-8 }}</ref> The star catalog of [[Hipparchus]] (2nd century BC) included 1020 stars and was used to assemble [[Ptolemy]]'s star catalogue.<ref>{{cite book
| first=Gerd | last=Grasshoff | year=1990
| title=The history of Ptolemy's star catalogue
| publisher=Springer | pages=1–5 | isbn=0-387-97181-5 }}</ref> Hipparchus is known for the discovery of the first recorded ''[[nova]]'' (new star).<ref>{{cite web
| first=Antonios D. | last=Pinotsis
| title=Astronomy in Ancient Rhodes
| publisher=Section of Astrophysics, Astronomy and Mechanics, Department of Physics, University of Athens | url=http://conferences.phys.uoa.gr/jets2008/historical.html
| accessdate=2009-06-02 }}</ref> Many of the constellations and star names in use today derive from Greek astronomy.
 
In spite of the apparent immutability of the heavens, [[Chinese astronomy|Chinese astronomers]] were aware that new stars could appear.<ref name="clark">{{cite conference
| last1=Clark | first1=D. H. | last2=Stephenson | first2=F. R.
| title=The Historical Supernovae
| booktitle=Supernovae: A survey of current research; Proceedings of the Advanced Study Institute
| pages=355–370
| publisher=Dordrecht, D. Reidel Publishing Co
| date=June 29, 1981 | location=Cambridge, England
| bibcode=1982sscr.conf..355C
}}</ref> In 185 AD, they were the first to observe and write about a [[supernova]], now known as the [[SN 185]].<ref>{{cite journal
| last1=Zhao | first1=Fu-Yuan | last2=Strom | first2=R. G. | last3=Jiang | first3=Shi-Yang
| title=The Guest Star of AD185 Must Have Been a Supernova
| journal=Chinese Journal of Astronomy and Astrophysics
| year=2006 | volume=6 | issue=5 | pages=635–640 | doi=10.1088/1009-9271/6/5/17 |bibcode = 2006ChJAA...6..635Z }}</ref> The brightest stellar event in recorded history was the [[SN 1006]] supernova, which was observed in 1006 and written about by the Egyptian astronomer [[Ali ibn Ridwan]] and several Chinese astronomers.<ref>{{cite web
| date=March 5, 2003
| url=http://www.noao.edu/outreach/press/pr03/pr0304.html
| title=Astronomers Peg Brightness of History's Brightest Star
| publisher=NAOA News | accessdate=2006-06-08 }}</ref> The [[SN 1054]] supernova, which gave birth to the [[Crab Nebula]], was also observed by Chinese and Islamic astronomers.<ref name="SN1054">{{cite web
| last1=Frommert | first1=Hartmut | last2=Kronberg | first2=Christine
| date=August 30, 2006 | work=SEDS
| publisher=University of Arizona
| title=Supernova 1054 – Creation of the Crab Nebula
| url=http://messier.seds.org/more/m001_sn.html
}}</ref><ref name="PASP1942">{{cite journal
| last=Duyvendak | first=J. J. L.
| title=Further Data Bearing on the Identification of the Crab Nebula with the Supernova of 1054 A.D. Part I. The Ancient Oriental Chronicles
| journal=Publications of the Astronomical Society of the Pacific | volume=54 | issue=318 | pages=91–94
|date=April 1942 | bibcode=1942PASP...54...91D
| doi=10.1086/125409 }}<br />
{{Cite journal
| last=Mayall | first=N. U. | last2=Oort |first2=Jan Hendrik
| title=Further Data Bearing on the Identification of the Crab Nebula with the Supernova of 1054 A.D. Part II. The Astronomical Aspects
| journal=Publications of the Astronomical Society of the Pacific | volume=54 | issue=318 | pages=95–104 |date=April 1942 | bibcode=1942PASP...54...95M
| doi=10.1086/125410
}}</ref><ref>{{cite journal | display-authors=1
| last1=Brecher | first1=K. | last2=Fesen | first2=R. A.
| last3=Maran | first3=S. P. | last4=Brandt | first4=J. C. | year=1983
| title=Ancient records and the Crab Nebula supernova
| journal=The Observatory | volume=103 | pages=106–113
| bibcode=1983Obs...103..106B }}</ref>
 
[[Astronomy in medieval Islam|Medieval Islamic astronomers]] gave [[List of Arabic star names|Arabic names to many stars]] that are still used today, and they invented numerous [[Astronomy in medieval Islam#Instruments|astronomical instruments]] that could compute the positions of the stars. They built the first large [[observatory]] research institutes, mainly for the purpose of producing ''[[Zij]]'' star catalogues.<ref>{{cite journal
|last=Kennedy |first=Edward S. |year=1962
|title=Review: ''The Observatory in Islam and Its Place in the General History of the Observatory'' by Aydin Sayili
|journal=[[Isis (journal)|Isis]] |volume=53
|issue=2 |pages=237–239 |doi=10.1086/349558 }}</ref> Among these, the ''[[Book of Fixed Stars]]'' (964) was written by the [[Persian people|Persian]] astronomer [[Abd al-Rahman al-Sufi]], who observed a number of stars, [[star cluster]]s (including the [[Omicron Velorum]] and [[Brocchi's Cluster]]s) and [[galaxy|galaxies]] (including the [[Andromeda Galaxy]]).<ref name=Jones>{{cite book
| title=Messier's nebulae and star clusters
| url=http://books.google.cz/books?id=IuhLR35I9QUC&pg=&dq#v=onepage&q=&f
| first=Kenneth Glyn | last=Jones
| publisher=[[Cambridge University Press]]
| year=1991 | isbn=0-521-37079-5 | page=1 }}</ref> According to A. Zahoor, in the 11th century, the Persian [[polymath]] scholar [[Abu Rayhan Biruni]] described the [[Milky Way]] galaxy as a multitude of fragments having the properties of [[nebula|nebulous]] stars, and also gave the [[latitude]]s of various stars during a [[lunar eclipse]] in 1019.<ref>{{cite web
| last=Zahoor | first=A. | year=1997
| url=http://www.unhas.ac.id/~rhiza/saintis/biruni.html
| archiveurl=http://web.archive.org/web/20080626074150/http://www.unhas.ac.id/~rhiza/saintis/biruni.html
| archivedate=2008-06-26
| title=Al-Biruni | publisher=Hasanuddin University
| accessdate=2007-10-21 }}</ref>
 
According to Josep Puig, the [[Al-Andalus|Andalusian]] astronomer [[Ibn Bajjah]] proposed that the Milky Way was made up of many stars which almost touched one another and appeared to be a continuous image due to the effect of [[refraction]] from sublunary material, citing his observation of the [[conjunction (astronomy and astrology)|conjunction]] of Jupiter and Mars on 500 [[Islamic calendar|AH]] (1106/1107 AD) as evidence.<ref name=Montada>{{cite web
| first=Josep Puig | last=Montada
| title=Ibn Bajja | publisher=[[Stanford Encyclopedia of Philosophy]]
| url= http://plato.stanford.edu/entries/ibn-bajja
| date=September 28, 2007 | accessdate=2008-07-11 }}</ref> <!--
[[File:Andromedaurania.jpg|thumb|[[Andromeda (constellation)|Andromeda]] as depicted in ''Urania's Mirror'', set of [[constellation]] cards published in London c.1825]] -->
Early [[Europe]]an astronomers such as [[Tycho Brahe]] identified new stars in the night sky (later termed ''novae''), suggesting that the heavens were not immutable. In 1584 [[Giordano Bruno]] suggested that the stars were like the Sun, and may have [[Extrasolar planet|other planets]], possibly even Earth-like, in orbit around them,<ref name="he history">{{cite web
| last=Drake | first=Stephen A. | date=August 17, 2006
| url=http://heasarc.gsfc.nasa.gov/docs/heasarc/headates/heahistory.html
| title=A Brief History of High-Energy (X-ray & Gamma-Ray) Astronomy
| publisher=NASA HEASARC | accessdate=2006-08-24
}}</ref> an idea that had been suggested earlier by the ancient [[Greek philosophy|Greek philosophers]], [[Democritus]] and [[Epicurus]],<ref>{{cite web
| first1=Peter | last1=Greskovic | first2=Peter | last2=Rudy
| date=July 24, 2006 | url = http://www.eso.org/public/outreach/eduoff/cas/cas2004/casreports-2004/rep-228/
| title=Exoplanets | publisher=ESO
| accessdate=2012-06-15 }}</ref> and by medieval [[Islamic cosmology|Islamic cosmologists]]<ref>{{cite journal
| title=The impact of the Qur'anic conception of astronomical phenomena on Islamic civilization
| first=I. A. | last=Ahmad | journal=Vistas in Astronomy
| volume=39 | issue=4 | year=1995
| pages=395–403 [402]
| doi=10.1016/0083-6656(95)00033-X |bibcode = 1995VA.....39..395A }}</ref> such as [[Fakhr al-Din al-Razi]].<ref name=Setia>{{cite journal
| title=Fakhr Al-Din Al-Razi on Physics and the Nature of the Physical World: A Preliminary Survey
| first=Adi | last=Setia | journal=Islam & Science
| volume=2 | year=2004 | url= http://findarticles.com/p/articles/mi_m0QYQ/is_2_2/ai_n9532826/
| accessdate=2010-03-02}}</ref> By the following century, the idea of the stars being the same as the Sun was reaching a consensus among astronomers. To explain why these stars exerted no net gravitational pull on the Solar System, [[Isaac Newton]] suggested that the stars were equally distributed in every direction, an idea prompted by the theologian [[Richard Bentley]].<ref>{{cite web
| last=Hoskin | first=Michael | year=1998
| url=http://www.stsci.edu/stsci/meetings/lisa3/hoskinm.html
| title=The Value of Archives in Writing the History of Astronomy
| publisher=Space Telescope Science Institute
| accessdate=2006-08-24 }}</ref>
 
The Italian astronomer [[Geminiano Montanari]] recorded observing variations in luminosity of the star [[Algol]] in 1667. [[Edmond Halley]] published the first measurements of the [[proper motion]] of a pair of nearby "fixed" stars, demonstrating that they had changed positions from the time of the ancient [[Ancient Greece|Greek]] astronomers [[Ptolemy]] and [[Hipparchus]].<ref name="he history" />
 
[[William Herschel]] was the first astronomer to attempt to determine the distribution of stars in the sky. During the 1780s, he performed a series of gauges in 600 directions, and counted the stars observed along each line of sight. From this he deduced that the number of stars steadily increased toward one side of the sky, in the direction of the [[Milky Way]] [[Galactic Center|core]]. His son [[John Herschel]] repeated this study in the southern hemisphere and found a corresponding increase in the same direction.<ref>{{cite journal
| last=Proctor | first=Richard A.
| title=Are any of the nebulæ star-systems? | journal=Nature
| year=1870 | pages=331–333
| url=http://digicoll.library.wisc.edu/cgi-bin/HistSciTech/HistSciTech-idx?type=div&did=HISTSCITECH.0012.0052.0005&isize=M
| issue=13
| doi=10.1038/001331a0 | volume=1 |bibcode = 1870Natur...1..331P }}</ref> In addition to his other accomplishments, William Herschel is also noted for his discovery that some stars do not merely lie along the same line of sight, but are also physical companions that form [[binary star]] systems.
 
The science of [[astronomical spectroscopy|stellar spectroscopy]] was pioneered by [[Joseph von Fraunhofer]] and [[Angelo Secchi]]. By comparing the spectra of stars such as [[Sirius]] to the Sun, they found differences in the strength and number of their [[Spectral line|absorption lines]]—the dark lines in a stellar spectra due to the absorption of specific frequencies by the atmosphere. In 1865 Secchi began classifying stars into [[Stellar classification|spectral types]].<ref>{{cite web
| last=MacDonnell | first=Joseph
| url=http://www.faculty.fairfield.edu/jmac/sj/scientists/secchi.htm
| archiveurl=http://web.archive.org/web/20110721210124/http://www.faculty.fairfield.edu/jmac/sj/scientists/secchi.htm
| archivedate=2011-07-21
| title=Angelo Secchi, S.J. (1818–1878) the Father of Astrophysics
| publisher=[[Fairfield University]]
| accessdate=2006-10-02}}</ref> However, the modern version of the stellar classification scheme was developed by [[Annie Jump Cannon|Annie J. Cannon]] during the 1900s.
[[File:Alpha Centauri AB over limb of Saturn PIA10406.jpg|thumb|300px|left|Alpha Centauri A and B over limb of Saturn</center>]]
 
The first direct measurement of the distance to a star ([[61 Cygni]] at 11.4 [[light-years]]) was made in 1838 by [[Friedrich Bessel]] using the [[parallax]] technique. Parallax measurements demonstrated the vast separation of the stars in the heavens.<ref name="he history" /> Observation of double stars gained increasing importance during the 19th century. In 1834, Friedrich Bessel observed changes in the proper motion of the star Sirius, and inferred a hidden companion. [[Edward Charles Pickering|Edward Pickering]] discovered the first [[spectroscopic binary]] in 1899 when he observed the periodic splitting of the spectral lines of the star [[Mizar (star)|Mizar]] in a 104-day period. Detailed observations of many binary star systems were collected by astronomers such as [[Friedrich Georg Wilhelm von Struve|William Struve]] and [[Sherburne Wesley Burnham|S. W. Burnham]], allowing the masses of stars to be determined from computation of the [[orbital elements]]. The first solution to the problem of deriving an orbit of binary stars from telescope observations was made by Felix Savary in 1827.<ref>{{cite book
| first=Robert G. | last=Aitken | title=The Binary Stars | page=66
| publisher=Dover Publications Inc. | location=New York
| year=1964 | isbn=0-486-61102-7 }}</ref>
The twentieth century saw increasingly rapid advances in the scientific study of stars. The [[photograph]] became a valuable astronomical tool. [[Karl Schwarzschild]] discovered that the color of a star, and hence its temperature, could be determined by comparing the [[visual magnitude]] against the [[photographic magnitude]]. The development of the [[photoelectric]] [[photometer]] allowed very precise measurements of magnitude at multiple wavelength intervals. In 1921 [[Albert Abraham Michelson|Albert A. Michelson]] made the first measurements of a stellar diameter using an [[interferometer]] on the [[Mount Wilson Observatory|Hooker telescope]].<ref>{{cite journal
| last1=Michelson | first1=A. A. | last2=Pease | first2=F. G.
| title=Measurement of the diameter of Alpha Orionis with the interferometer
| journal=Astrophysical Journal | year=1921 | volume=53 | pages=249–259
| bibcode=1921ApJ....53..249M | doi = 10.1086/142603
}}</ref>
 
Important theoretical work on the physical structure of stars occurred during the first decades of the twentieth century. In 1913, the [[Hertzsprung-Russell diagram]] was developed, propelling the astrophysical study of stars. Successful models were developed to explain the interiors of stars and stellar evolution. [[Cecilia Payne-Gaposchkin]] first proposed that stars were made primarily of hydrogen and helium in her 1925 PhD thesis.<ref>{{cite web
| url=http://cwp.library.ucla.edu/Phase2/Payne-Gaposchkin,_Cecilia_Helena@861234567.html
| title=" Payne-Gaposchkin, Cecilia Helena." CWP
| publisher=[[University of California]]
| accessdate=2013-02-21}}</ref> The spectra of stars were further understood through advances in [[quantum mechanics|quantum physics]]. This allowed the chemical composition of the stellar atmosphere to be determined.<ref name="new cosmos">{{cite book
| last1=Unsöld | first1=Albrecht | title=The New Cosmos
| publisher=Springer | location=New York
| year=2001 | edition=5th | pages=180–185, 215–216
| isbn=3-540-67877-8 }}</ref>
 
With the exception of [[supernova]]e, individual stars have primarily been observed in our [[Local Group]] of [[galaxy|galaxies]],<ref>e. g. {{cite journal
| last1=Battinelli | first1=Paolo | last2=Demers | first2=Serge
| last3=Letarte | first3=Bruno
| title=Carbon Star Survey in the Local Group. V. The Outer Disk of M31
| journal=The Astronomical Journal
| year=2003 | volume=125 | issue=3 | pages=1298–1308
| bibcode=2003AJ....125.1298B | doi = 10.1086/346274
}}</ref> and especially in the visible part of the [[Milky Way]] (as demonstrated by the detailed [[star catalogue]]s available for our
galaxy).<ref>{{cite news
| title=Millennium Star Atlas marks the completion of ESA's Hipparcos Mission
| publisher=ESA | date=December 8, 1997
| url=http://www.rssd.esa.int/index.php?project=HIPPARCOS&page=esa_msa
| accessdate=2007-08-05 }}</ref> But some stars have been observed in the M100 galaxy of the [[Virgo Cluster]], about 100 million light years from the Earth.<ref>{{cite web
| last1=Villard | first1=Ray | last2=Freedman | first2=Wendy L.
| date=October 26, 1994
| url=http://hubblesite.org/newscenter/archive/releases/1994/1994/49/text/
| title=Hubble Space Telescope Measures Precise Distance to the Most Remote Galaxy Yet
| publisher=Hubble Site
| accessdate = 2007-08-05 }}</ref> In the [[Local Supercluster]] it is possible to see star clusters, and current telescopes could in principle observe faint individual stars in the [[Local Cluster]]<ref>{{cite news
| title=Hubble Completes Eight-Year Effort to Measure Expanding Universe
| publisher=Hubble Site | date=May 25, 1999
| url=http://hubblesite.org/newscenter/archive/releases/1999/19/text/
| accessdate=2007-08-02 }}</ref> (see [[Cepheids]]). However, outside the [[Local Supercluster]] of galaxies, neither individual stars nor clusters of stars have been observed. The only exception is a faint image of a large star cluster containing hundreds of thousands of stars located at a distance of one billion light years<ref>{{cite news
| title=UBC Prof., alumnus discover most distant star clusters: a billion light-years away.
| publisher=UBC Public Affairs | date=January 8, 2007
| url=http://www.publicaffairs.ubc.ca/media/releases/2007/mr-07-001.html
| accessdate=2007-08-02 }}</ref>—ten times further than the most distant star cluster previously observed.
 
==Designations==
{{Main|Star designation|Astronomical naming conventions|Star catalogue}}
The concept of the constellation was known to exist during the [[Babylon]]ian period. Ancient sky watchers imagined that prominent arrangements of stars formed patterns, and they associated these with particular aspects of nature or their myths. Twelve of these formations lay along the band of the [[ecliptic]] and these became the basis of [[astrology]].<ref name=koch95/> Many of the more prominent individual stars were also given names, particularly with [[Arab language|Arabic]] or [[Latin language|Latin]] designations.
 
As well as certain constellations and the Sun itself, individual stars have their own [[mythology|myth]]s.<ref name="mythology">{{cite web
| last = Coleman | first = Leslie S
| url = http://frostydrew.org/papers.dc/papers/paper-myths/
| title = Myths, Legends and Lore
| publisher = Frosty Drew Observatory
| accessdate = 2012-06-15 }}</ref> To the [[Ancient Greek religion|Ancient Greek]]s, some "stars", known as [[planet]]s (Greek πλανήτης (planētēs), meaning "wanderer"), represented various important deities, from which the names of the planets [[Mercury (planet)|Mercury]], [[Venus]], [[Mars]], [[Jupiter]] and [[Saturn]] were taken.<ref name="mythology" /> ([[Uranus]] and [[Neptune]] were also [[Greek mythology|Greek]] and [[Roman mythology|Roman gods]], but neither planet was known in Antiquity because of their low brightness. Their names were assigned by later astronomers.)
 
Circa 1600, the names of the constellations were used to name the stars in the corresponding regions of the sky. The German astronomer [[Johann Bayer]] created a series of star maps and applied Greek letters as [[Bayer designation|designations]] to the stars in each constellation. Later a numbering system based on the star's [[right ascension]] was invented and added to [[John Flamsteed]]'s star catalogue in his book ''"Historia coelestis Britannica"'' (the 1712 edition), whereby this numbering system came to be called ''[[Flamsteed designation]]'' or ''Flamsteed numbering''.<ref>{{cite web
| url = http://www.iau.org/public/naming/ | title = Naming Astronomical Objects
| publisher = [[International Astronomical Union]] (IAU)
| accessdate = 2009-01-30 }}</ref><ref>{{cite web
| url = http://spider.seds.org/spider/Misc/naming.html | title = Naming Stars
| publisher = [[Students for the Exploration and Development of Space]] (SEDS)
| accessdate = 2009-01-30 }}</ref>
 
The only internationally recognized authority for naming celestial bodies is the [[International Astronomical Union]] (IAU).<ref name=space_law09/> A number of private companies sell names of stars, which the [[British Library]] calls an [[regulation|unregulated]] [[commercial enterprise]].<ref name=astrometry05/><ref name=bl_disclaimer/> However, the IAU has disassociated itself from this commercial practice, and these names are neither recognized by the IAU nor used by them.<ref name=andersen10/> One such star naming company is the [[International Star Registry]], which, during the 1980s, was accused of [[deceptive practice]] for making it appear that the assigned name was [[Official#Adjective|official]]. This now-discontinued ISR practice was informally labeled a scam and a fraud,<ref name=si30_5/><ref name=sd19980401/><ref name=golden_faflick82/><ref name=di_justo20011226/> and the [[New York City Department of Consumer Affairs]] issued a violation against ISR for engaging in a deceptive trade practice.<ref name=pliat02/><ref name=sclafani19980508/>
 
==Units of measurement==
Although stellar parameters can be expressed in [[International System of Units|SI units]] or [[CGS unit]]s, it is often most convenient to express mass, luminosity, and [[radius|radii]] in solar units, based on the characteristics of the Sun:
 
:{|
| [[solar mass]]:
| ''M''<sub>⊙</sub> = {{nowrap|1.9891 × 10<sup>30</sup> [[kilogram|kg]]}}<ref name="constants">{{cite journal
  | last1=Sackmann | first1=I.-J. | last2=Boothroyd | first2=A. I.
  | title=Our Sun. V. A Bright Young Sun Consistent with Helioseismology and Warm Temperatures on Ancient Earth and Mars
  | journal=The Astrophysical Journal | year=2003 | volume=583
| issue=2 | pages=1024–1039 | bibcode=2003ApJ...583.1024S
  | doi=10.1086/345408 |arxiv = astro-ph/0210128 }}</ref>
|-
| [[solar luminosity]]:
| ''L''<sub>⊙</sub> = {{nowrap|3.827 × 10<sup>26</sup> [[watt]]s}}<ref name="constants" />
|-
| [[solar radius]]
| ''R''<sub>⊙</sub> = {{nowrap|6.960 × 10<sup>8</sup> [[Metre|m]]}}<ref>{{cite journal
| last1=Tripathy | first1=S. C. | last2=Antia | first2=H. M.
| title=Influence of surface layers on the seismic estimate of the solar radius
| journal=Solar Physics | year=1999
| volume=186 | issue=1/2 | pages=1–11
| bibcode=1999SoPh..186....1T | doi = 10.1023/A:1005116830445
}}</ref>
|}
 
Large lengths, such as the radius of a giant star or the [[semi-major axis]] of a binary star system, are often expressed in terms of the [[astronomical unit]] (AU)—approximately the mean distance between the Earth and the Sun (150 million km or 93 million miles).
 
==Formation and evolution==
{{Main|Stellar evolution}}
 
Stars are formed within extended regions of higher density in the [[interstellar medium]], although the density is still lower than the inside of a [[vacuum chamber]]. These regions are called ''[[molecular cloud]]s'' and consist mostly of hydrogen, with about 23–28% helium and a few percent heavier elements. One example of such a star-forming region is the [[Orion Nebula]].<ref>
{{cite journal
| last=Woodward | first=P. R.
| title=Theoretical models of star formation
| journal=Annual review of astronomy and astrophysics
| year=1978 | volume=16
| issue=1 | pages=555–584 | doi = 10.1146/annurev.aa.16.090178.003011
| bibcode=1978ARA&A..16..555W
}}</ref> As massive stars are formed from molecular clouds, they powerfully illuminate those clouds. They also [[ion]]ize the hydrogen, creating an [[H II region]].
 
All stars spend the majority of their lives as ''[[main sequence]] stars'', fueled primarily by the nuclear fusion of hydrogen into helium within their cores. However, stars of different masses have markedly different properties at various stages of their lives. The ultimate fate of more massive stars is different from that of less massive stars, as is their [[luminosity]] and the impact they have on their environment. Therefore, stars are often grouped by mass. ''Very low mass stars'' with masses below 0.5 [[solar masses]] do not enter the [[asymptotic giant branch]] (AGB) but evolve directly into white dwarfs. ''Low mass stars'' (including the Sun) with a mass above about 0.5 and below about 1.8–2.2 solar masses (depending on composition) do enter the AGB, where they develop a degenerate helium core. ''Intermediate-mass stars'' undergo [[helium fusion]] and develop a degenerate carbon-oxygen core. ''Massive stars'' have a minimum mass of 7–10 solar masses, but this may be as low as 5–6 solar masses. These stars undergo [[Carbon burning process|carbon fusion]], with their lives ending in a core-collapse [[supernova]] explosion.<ref>{{cite book
| first=Sun | last=Kwok | year=2000 | pages=103–104
| title=The origin and evolution of planetary nebulae
| volume=33 | series=Cambridge astrophysics series
| publisher=Cambridge University Press | isbn=0-521-62313-8 }}</ref>
 
===Protostar formation===
{{Main|Star formation}}
The formation of a star begins with gravitational instability within a molecular cloud, caused by regions of higher density often triggered by shock waves from nearby [[supernova]]e (massive stellar explosions), the collision of different molecular clouds, or the collision of [[galaxy|galaxies]] (as in a [[starburst galaxy]]). Once a region reaches a sufficient density of matter to satisfy the criteria for [[Jeans instability]], it begins to collapse under its own gravitational force.<ref>{{cite book
| first=Michael David | last=Smith | year=2004
| title=The Origin of Stars | publisher=Imperial College Press
| isbn=1-86094-501-5 | pages=57–68 }}</ref>
[[File:Witness the Birth of a Star.jpg|thumb|right|300px|Artist's conception of the birth of a star within a dense [[molecular cloud]]. ''NASA image'']]
 
As the cloud collapses, individual conglomerations of dense dust and gas form what are known as [[Bok globule]]s. As a globule collapses and the density increases, the gravitational energy is converted into heat and the temperature rises. When the protostellar cloud has approximately reached the stable condition of [[hydrostatic equilibrium]], a [[protostar]] forms at the core.<ref>{{cite web
| last = Seligman | first = Courtney
| url = http://courtneyseligman.com/text/stars/starevol2.htm
| archiveurl = http://web.archive.org/web/20080623190408/http://courtneyseligman.com/text/stars/starevol2.htm
| archivedate = 2008-06-23
| title = Slow Contraction of Protostellar Cloud | work=Self-published
| accessdate = 2006-09-05 }}</ref> These [[pre–main sequence star]]s are often surrounded by a [[protoplanetary disk]] and powered mainly by the release of gravitational energy. The period of gravitational contraction lasts about 10–15 million years.
 
Early stars of less than 2 solar masses are called [[T Tauri star]]s, while those with greater mass are [[Herbig Ae/Be star]]s. These newly born stars emit jets of gas along their axis of rotation, which may reduce the [[angular momentum]] of the collapsing star and result in small patches of nebulosity known as [[Herbig–Haro object]]s.<ref>{{cite conference
| last1=Bally | first1=J. | last2=Morse | first2=J.
| last3=Reipurth | first3=B. | year = 1996
| title=The Birth of Stars: Herbig-Haro Jets, Accretion and Proto-Planetary Disks
| booktitle = Science with the Hubble Space Telescope – II. Proceedings of a workshop held in Paris, France, December 4–8, 1995
| editor1-last=Benvenuti | editor1-first=Piero
| editor2-first=F. D. | editor2-last=Macchetto
| editor3-first=Ethan J. | editor3-last=Schreier
| publisher=Space Telescope Science Institute | page=491
| bibcode=1996swhs.conf..491B
}}</ref><ref name=smith04>{{cite book
| first=Michael David | last=Smith
| title=The origin of stars | page=176 | year=2004
| isbn=1-86094-501-5
| publisher=Imperial College Press
}}</ref> These jets, in combination with radiation from nearby massive stars, may help to drive away the surrounding cloud from which the star was formed.<ref>{{cite news
| first=Tom | last=Megeath | date=May 11, 2010
| title=Herschel finds a hole in space
| url=http://www.esa.int/esaCP/SEMFEAKPO8G_index_0.html
| publisher=ESA | accessdate=2010-05-17 }}</ref>
 
Early in their life, T Tauri stars follow the [[Hayashi track]]—they contract and decrease in luminosity while remaining at roughly the same temperature.  Less massive T Tauri stars follow this track to the main sequence, while more massive stars turn onto the [[Henyey track]].
 
===Main sequence===
{{Main|Main sequence}}
Stars spend about 90% of their lifetime fusing hydrogen into helium in high-temperature and high-pressure reactions near the core. Such stars are said to be on the [[main sequence]] and are called dwarf stars. Starting at zero-age main sequence, the proportion of helium in a star's core will steadily increase, the rate of nuclear fusion at the core will slowly increase, as will the star's temperature and luminosity.<ref>{{cite journal | display-authors=1
| last1=Mengel | first1=J. G. | last2=Demarque | first2=P.
| last3=Sweigart | first3=A. V. | last4=Gross | first4=P. G.
| title=Stellar evolution from the zero-age main sequence
| journal=Astrophysical Journal Supplement Series
| year=1979 | volume=40 | pages=733–791
| bibcode=1979ApJS...40..733M | doi = 10.1086/190603
}}</ref> The Sun, for example, is estimated to have increased in luminosity by about 40% since it reached the main sequence 4.6 billion (4.6 × 10<sup>9</sup>) years ago.<ref name=sun_future />
 
Every star generates a [[stellar wind]] of particles that causes a continual outflow of gas into space. For most stars, the mass lost is negligible. The Sun loses 10<sup>−14</sup> solar masses every year,<ref>{{cite journal | display-authors=1
| last1=Wood | first1=B. E. | last2=Müller | first2=H.-R.
| last3=Zank | first3=G. P. | last4=Linsky | first4=J. L.
| title=Measured Mass-Loss Rates of Solar-like Stars as a Function of Age and Activity
| journal=The Astrophysical Journal | year=2002
| volume=574 | issue=1 | pages=412–425
| doi = 10.1086/340797 | bibcode=2002ApJ...574..412W
|arxiv = astro-ph/0203437 }}</ref> or about 0.01% of its total mass over its entire lifespan. However, very massive stars can lose 10<sup>−7</sup> to 10<sup>−5</sup> solar masses each year, significantly affecting their evolution.<ref>{{cite journal
| last1=de Loore | first1=C. | last2=de Greve | first2=J. P.
| last3=Lamers | first3=H. J. G. L. M.
| title=Evolution of massive stars with mass loss by stellar wind
| journal=Astronomy and Astrophysics | year=1977 | volume=61
| issue=2 | pages=251–259
| bibcode=1977A&A....61..251D }}</ref> Stars that begin with more than 50 solar masses can lose over half their total mass while on the main sequence.<ref>{{cite web
| url = http://www.rmg.co.uk/explore/astronomy-and-time/astronomy-facts/stars/stellar-evolution/the-evolution-of-stars-between-50-and-100-times-the-mass-of-the-sun
| title = The evolution of stars between 50 and 100 times the mass of the Sun
| publisher = Royal Greenwich Observatory
| accessdate = 2006-09-07 }}</ref>
 
[[File:H-R diagram -edited-3.gif|right|thumb|360px|An example of a [[Hertzsprung–Russell diagram]] for a set of stars that includes the Sun (center). (See "Classification" below.)]]
The duration that a star spends on the main sequence depends primarily on the amount of fuel it has to fuse and the rate at which it fuses that fuel, i.e. its initial mass and its luminosity. For the Sun, its life is estimated to be about 10 billion (10<sup>10</sup>) years. Massive stars consume their fuel very rapidly and are short-lived. Low mass stars consume their fuel very slowly. Stars less massive than 0.25 solar masses, called [[red dwarf]]s, are able to fuse nearly all of their mass as fuel while stars of about 1 solar mass can only use about 10% of their mass as fuel. The combination of their slow fuel consumption and relatively large usable fuel supply allows stars about 0.25 times the mass of the Sun to last for about one trillion (10<sup>12</sup>) years according to stellar evolution calculations, while the least-massive hydrogen-fusing stars (0.08 solar masses) will last for about 12 trillion years.<ref name=adams>{{cite conference
| last=Adams | first=Fred C.
| coauthors=Laughlin, Gregory; Graves, Genevieve J. M
| title=Red Dwarfs and the End of the Main Sequence
| booktitle=Gravitational Collapse: From Massive Stars to Planets
| pages=46–49
| publisher=Revista Mexicana de Astronomía y Astrofísica
| url=http://www.astroscu.unam.mx/rmaa/RMxAC..22/PDF/RMxAC..22_adams.pdf
| accessdate = 2008-06-24 }}</ref> At the end of their lives, red dwarfs simply become dimmer and dimmer.<ref name="late stages" /> However, since the lifespan of such stars is greater than the current [[age of the universe]] (13.8 billion years), no stars under about 0.85 solar masses<ref name="saomainseq">{{cite web | title=Main Sequence Lifetime | url=http://astronomy.swin.edu.au/cosmos/M/Main+Sequence+Lifetime | work=Swinburne Astronomy Online Encyclopedia of Astronomy | publisher=Swinburne University of Technology }}</ref> are expected to have moved off of the main sequence.
 
Besides mass, the elements heavier than helium can play a significant role in the evolution of stars. In astronomy all elements heavier than helium are considered a "metal", and the chemical [[concentration]] of these elements is called the [[metallicity]]. The metallicity can influence the duration that a star will burn its fuel, control the formation of magnetic fields<ref>{{cite journal
| display-authors=1
| last1=Pizzolato | first1=N. | last2=Ventura | first2=P.
| last3=D'Antona | first3=F. | last4=Maggio | first4=A.
| last5=Micela | first5=G. | last6=Sciortino | first6=S.
| title=Subphotospheric convection and magnetic activity dependence on metallicity and age: Models and tests
| journal=Astronomy & Astrophysics
| year=2001 | volume=373
| issue=2 | pages=597–607
| doi=10.1051/0004-6361:20010626
| bibcode=2001A&A...373..597P}}</ref> and modify the strength of the stellar wind.<ref>{{cite web
| date = June 18, 2004
| url = http://www.star.ucl.ac.uk/groups/hotstar/research_massloss.html
| archiveurl = http://web.archive.org/web/20041122143115/http://www.star.ucl.ac.uk/groups/hotstar/research_massloss.html
| archivedate = 2004-11-22
| title = Mass loss and Evolution | publisher = UCL Astrophysics Group
| accessdate = 2006-08-26 }}</ref> Older, [[Stellar population|population II]] stars have substantially less metallicity than the younger, population I stars due to the composition of the molecular clouds from which they formed. Over time these clouds become increasingly enriched in heavier elements as older stars die and shed portions of their [[stellar atmosphere|atmospheres]].
 
===Post-main sequence===
{{Main|Red giant}}
As stars of at least 0.4 solar masses<ref name="late stages" /> exhaust their supply of hydrogen at their core, their outer layers expand greatly and cool to form a [[red giant]]. In about 5 billion years, when the Sun enters this phase, it will expand to a maximum radius of roughly {{convert|1|AU|e6km|lk=in|abbr=off}}, 250 times its present size. As a giant, the Sun will lose roughly 30% of its current mass.<ref name="sun_future">{{cite journal | last1=Sackmann | first1=I. J. | last2=Boothroyd | first2=A. I. | last3=Kraemer | first3=K. E. | title=Our Sun. III. Present and Future | page=457 | journal=Astrophysical Journal | year=1993 | volume=418 | bibcode=1993ApJ...418..457S | doi = 10.1086/173407}}</ref><ref name="sun_future_schroder">{{cite journal | first1=K.-P. | last1=Schröder | last2=Smith | first2=Robert Connon | year=2008 | title=Distant future of the Sun and Earth revisited | doi=10.1111/j.1365-2966.2008.13022.x | journal=Monthly Notices of the Royal Astronomical Society | volume = 386 | issue=1 | page = 155 | bibcode=2008MNRAS.386..155S|arxiv = 0801.4031 }} See also {{cite news
| url=http://www.newscientist.com/article/dn13369?feedId=online-news_rss20
| title=Hope dims that Earth will survive Sun's death
| date=February 22, 2008
| work=NewScientist.com news service
| first=Jason | last=Palmer
| accessdate=2008-03-24 }}</ref>
 
In a red giant of up to 2.25 solar masses, hydrogen fusion proceeds in a shell surrounding the core.<ref name="hinshaw">{{cite web
| last = Hinshaw | first = Gary | date = August 23, 2006
| url = http://map.gsfc.nasa.gov/universe/rel_stars.html
| title = The Life and Death of Stars
| publisher = NASA WMAP Mission | accessdate = 2006-09-01 }}</ref> Eventually the core is compressed enough to start [[helium fusion]], and the star now gradually shrinks in radius and its surface temperature increases. For larger stars, the core region transitions directly from fusing hydrogen to fusing helium.<ref name="iben"/>
 
After the star has consumed the helium at the core, fusion continues in a shell around a hot core of carbon and oxygen. The star then follows an evolutionary path that parallels the original red giant phase, but at a higher surface temperature.
 
====Massive stars====
{{Main|Red supergiant}}
[[File:Hubble Space Telescope picture of Betelgeuse.jpg|left|thumb|[[Betelgeuse]] is a red supergiant star approaching the end of its life cycle.]]
 
During their helium-burning phase, very high mass stars with more than nine solar masses expand to form [[red supergiant]]s. Once this fuel is exhausted at the core, they continue to fuse elements heavier than helium.
 
The core contracts until the temperature and pressure are sufficient to fuse [[carbon]] (see [[carbon burning process]]). This process continues, with the successive stages being fueled by [[neon]] (see [[neon burning process]]), [[oxygen]] (see [[oxygen burning process]]), and [[silicon]] (see [[silicon burning process]]). Near the end of the star's life, fusion continues along a series of onion-layer shells within the star. Each shell fuses a different element, with the outermost shell fusing hydrogen; the next shell fusing helium, and so forth.<ref>{{cite web | url = http://www.rmg.co.uk/explore/astronomy-and-time/astronomy-facts/stars/what-is-a-star | title = What is a star? | publisher = Royal Greenwich Observatory | accessdate = 2006-09-07 }}</ref>
 
The final stage is reached when a massive star begins producing [[iron]]. Since iron nuclei are more [[binding energy|tightly bound]] than any heavier nuclei, any fusion beyond iron does not produce a net release of energy—the process would, on the contrary, consume energy. Likewise, since they are more tightly bound than all lighter nuclei, energy cannot be released by [[Nuclear fission|fission]].<ref name="hinshaw" /> In relatively old, very massive stars, a large core of inert iron will accumulate in the center of the star. The heavier elements in these stars can work their way to the surface, forming evolved objects known as [[Wolf-Rayet star]]s that have a dense stellar wind which sheds the outer atmosphere.
 
====Collapse====
As a star's core shrinks, the intensity of radiation from that surface increases, creating such [[radiation pressure]] on the outer shell of gas that it will push those layers away, forming a [[planetary nebula]]. If what remains after the outer atmosphere has been shed is less than 1.4 solar masses, it shrinks to a relatively tiny object about the size of Earth, known as a [[white dwarf]]. It is not massive enough for further gravitational compression to take place.<ref>{{cite journal | last1=Liebert | first1=J. | title=White dwarf stars | journal=Annual review of astronomy and astrophysics | year=1980 | volume=18 | issue=2 | pages=363–398 | bibcode=1980ARA&A..18..363L | doi = 10.1146/annurev.aa.18.090180.002051}}</ref> The [[electron-degenerate matter]] inside a white dwarf is no longer a plasma, even though stars are generally referred to as being spheres of plasma. Eventually, white dwarfs will fade into [[black dwarf]]s over a very long period of time.
[[File:Crab Nebula.jpg|thumb|200px|right|The [[Crab Nebula]], remnants of a supernova that was first observed around 1050 AD]]
 
In larger stars, fusion continues until the iron core has grown so large (more than 1.4 solar masses) that it can no longer support its own mass. This core will suddenly collapse as its electrons are driven into its protons, forming neutrons, neutrinos and gamma rays in a burst of [[electron capture]] and [[inverse beta decay]]. The [[shock wave|shockwave]] formed by this sudden collapse causes the rest of the star to explode in a [[supernova]]. Supernovae are so bright that they may briefly outshine the star's entire home galaxy. When they occur within the Milky Way, supernovae have historically been observed by naked-eye observers as "new stars" where none seemingly existed before.<ref name="supernova">{{cite web
| date=April 6, 2006
| url=http://heasarc.gsfc.nasa.gov/docs/objects/snrs/snrstext.html
| title=Introduction to Supernova Remnants
| publisher=Goddard Space Flight Center
| accessdate=2006-07-16 }}</ref>
 
Most of the star's matter is blown away by the supernova explosion (forming nebulae such as the Crab Nebula).<ref name="supernova" /> What remains will be a [[neutron star]] (which sometimes manifests itself as a [[pulsar]] or [[X-ray burster]]) or, in the case of the largest stars (large enough to leave a remnant greater than roughly 4 solar masses), a [[black hole]].<ref>{{cite journal | last1=Fryer | first1=C. L. | title=Black-hole formation from stellar collapse | journal=Classical and Quantum Gravity | year=2003 | volume=20 | issue=10 | pages=S73–S80 | doi = 10.1088/0264-9381/20/10/309 | bibcode=2003CQGra..20S..73F}}</ref> In a neutron star the matter is in a state known as [[neutron-degenerate matter]], with a more exotic form of degenerate matter, [[QCD matter]], possibly present in the core. Within a black hole the matter is in a state that is not currently understood.
 
The blown-off outer layers of dying stars include heavy elements, which may be recycled during new star formation. These heavy elements allow the formation of rocky planets. The outflow from supernovae and the stellar wind of large stars play an important part in shaping the interstellar medium.<ref name="supernova" />
 
==Distribution==
[[File:Sirius A and B artwork.jpg|left|thumb|250px|A [[white dwarf]] star in orbit around [[Sirius]] (artist's impression). ''NASA image'']]
 
In addition to isolated stars, a [[multiple star|multi-star system]] can consist of two or more gravitationally bound stars that orbit each other. The simplest and most common multi-star system is a [[binary star]], but systems of three or more stars are also found. For reasons of orbital stability, such multi-star systems are often organized into hierarchical sets of binary stars.<ref>{{cite book
| first1=Victor G. | last1=Szebehely
| last2=Curran | first2=Richard B. | year=1985
| title=Stability of the Solar System and Its Minor Natural and Artificial Bodies
| publisher=Springer
| isbn=90-277-2046-0 }}</ref> Larger groups called [[star cluster]]s also exist. These range from loose [[stellar associations]] with only a few stars, up to enormous [[globular clusters]] with hundreds of thousands of stars.
 
It has been a long-held assumption that the majority of stars occur in gravitationally bound, multiple-star systems. This is particularly true for very massive O and B class stars, where 80% of the stars are believed to be part of multiple-star systems. However the proportion of single star systems increases for smaller stars, so that only 25% of red dwarfs are known to have stellar companions. As 85% of all stars are red dwarfs, most stars in the Milky Way are likely single from birth.<ref>{{cite press release
| publisher=Harvard-Smithsonian Center for Astrophysics
| date=January 30, 2006
| url=http://www.cfa.harvard.edu/news/2006/pr200611.html
| title=Most Milky Way Stars Are Single
| accessdate=2006-07-16 }}</ref>
 
Stars are not spread uniformly across the universe, but are normally grouped into galaxies along with interstellar gas and dust. A typical galaxy contains hundreds of billions of stars, and there are more than 100 billion (10<sup>11</sup>) galaxies in the [[observable universe]].<ref>{{cite web | title=What is a galaxy? How many stars in a galaxy / the Universe? | publisher=Royal Greenwich Observatory | url=http://www.rmg.co.uk/explore/astronomy-and-time/astronomy-facts/faqs/what-is-a-galaxy-how-many-stars-in-a-galaxy-how-many-stars/galaxies-in-the-universe | accessdate=2006-07-18 }}</ref> A 2010 star count estimate was 300 [[sextillion]] ({{nowrap|3 × 10<sup>23</sup>}}) in the observable universe.<ref>{{cite news
| first=Seth | last=Borenstein | date=December 1, 2010
| title=Universe's Star Count Could Triple | work=CBS News
| url=http://www.cbsnews.com/stories/2010/12/01/tech/main7107200.shtml | accessdate=2011-07-14}}</ref>
While it is often believed that stars only exist within galaxies, intergalactic stars have been discovered.<ref>{{cite news
| title=Hubble Finds Intergalactic Stars
| publisher=Hubble News Desk | date=January 14, 1997
| url=http://hubblesite.org/newscenter/archive/releases/1997/02/text/
| accessdate=2006-11-06 }}</ref>
 
The nearest star to the Earth, apart from the Sun, is [[Proxima Centauri]], which is 39.9 trillion kilometres, or 4.2 light-years away. Travelling at the orbital speed of the [[Space Shuttle]] (8 kilometres per second—almost 30,000 kilometres per hour), it would take about 150,000 years to get there.<ref>3.99 × 10<sup>13</sup> km / (3 × 10<sup>4</sup> km/h × 24 × 365.25) = 1.5 × 10<sup>5</sup> years.</ref> Distances like this are typical inside [[disc (galaxy)|galactic discs]], including in the vicinity of the solar system.<ref>{{cite journal | last1=Holmberg | first1=J. | last2=Flynn | first2=C. | title=The local density of matter mapped by Hipparcos | journal=Monthly Notices of the Royal Astronomical Society | volume=313 | issue=2 | year=2000 | pages=209–216 | bibcode=2000MNRAS.313..209H | doi = 10.1046/j.1365-8711.2000.02905.x |arxiv = astro-ph/9812404 }}</ref> Stars can be much closer to each other in the centres of galaxies and in [[globular cluster]]s, or much farther apart in [[galactic spheroid|galactic halo]]s.
 
Due to the relatively vast distances between stars outside the galactic nucleus, collisions between stars are thought to be rare. In denser regions such as the core of globular clusters or the galactic center, collisions can be more common.<ref name="DarkMatter">{{cite news | title=Astronomers: Star collisions are rampant, catastrophic | publisher=CNN News | date=June 2, 2000 | url=http://archive.is/8lKf | accessdate=2014-01-21 }}</ref> Such collisions can produce what are known as [[blue straggler]]s. These abnormal stars have a higher surface temperature than the other main sequence stars with the same luminosity in the cluster.<ref>{{cite journal | display-authors=1 | first1=J. C. | last1=Lombardi, Jr. | last2=Warren | first2=J. S. | last3=Rasio | first3=F. A. | last4=Sills | first4=A. | last5=Warren | first5=A. R. | title = Stellar Collisions and the Interior Structure of Blue Stragglers | journal=The Astrophysical Journal | year=2002 | volume=568 | issue = 2 | pages=939–953 | bibcode=2002ApJ...568..939L | doi = 10.1086/339060|arxiv = astro-ph/0107388 }}</ref>
 
==Characteristics==
[[File:The sun1.jpg|thumb|right|The [[Sun]] is the nearest star to [[Earth]].]]
Almost everything about a star is determined by its initial mass, including essential characteristics such as luminosity and size, as well as its evolution, lifespan, and eventual fate.
 
===Age===
Most stars are between 1 billion and 10 billion years old. Some stars may even be close to 13.8 billion years old—the observed [[age of the universe]]. The oldest star yet discovered, [[HE 1523-0901|HE&nbsp;1523-0901]], is an estimated 13.2 billion years old.<ref>{{cite news | display-authors=1
| last1=Frebel | first1=A. | last2=Norris | first2=J. E. | last3=Christlieb | first3=N. | last4=Thom | first4=C. | last5=Beers | first5=T. C. | last6=Rhee | first6=J
| title=Nearby Star Is A Galactic Fossil
| publisher=Science Daily | date=May 11, 2007
| url=http://www.sciencedaily.com/releases/2007/05/070510151902.htm
| accessdate=2007-05-10
}}</ref><ref>{{cite journal | display-authors=1
| last1=Frebel | first1=Anna | last2=Christlieb | first2=Norbert
| last3=Norris | first3=John E. | last4=Thom | first4=Christopher
| last5=Beers | first5=Timothy C. | last6=Rhee | first6=Jaehyon
| title=Discovery of HE 1523-0901, a Strongly r-Process-enhanced Metal-poor Star with Detected Uranium
| journal=[[Astrophysical Journal]] Letters| volume=660 | issue=2
| pages=L117–L120 | date=May 2007 | doi=10.1086/518122
| bibcode=2007ApJ...660L.117F | arxiv=astro-ph/0703414  }}</ref>
 
The more massive the star, the shorter its lifespan, primarily because massive stars have greater pressure on their cores, causing them to burn hydrogen more rapidly. The most massive stars last an average of a few million years, while stars of minimum mass (red dwarfs) burn their fuel very slowly and last tens to hundreds of billions of years.<ref>{{cite web
| last1=Naftilan | first1=S. A. | last2=Stetson | first2=P. B.
| date=July 13, 2006
| url=http://www.scientificamerican.com/article.cfm?id=how-do-scientists-determi
| title=How do scientists determine the ages of stars? Is the technique really accurate enough to use it to verify the age of the universe?
| publisher=Scientific American
| accessdate=2007-05-11 }}</ref><ref>{{cite journal
| last1=Laughlin | first1=G. | last2=Bodenheimer | first2=P.
| last3=Adams | first3=F. C.
| title=The End of the Main Sequence
| journal=The Astrophysical Journal
| year=1997 | volume=482 | issue=1 | pages=420–432
| bibcode=1997ApJ...482..420L | doi = 10.1086/304125 }}</ref>
 
===Chemical composition===
{{See also|Metallicity|Molecules in stars}}
{{quote|“From a chemist’s point of view, the surface or interior of a star…is boring—there are no molecules there.”--[[Roald Hoffmann]]<ref>[http://www.americanscientist.org/issues/pub/stellar-molecules Stellar Molecules » American Scientist<!-- Bot generated title -->]</ref>}}
 
When stars form in the present Milky Way galaxy they are composed of about 71% hydrogen and 27% helium,<ref>{{cite book
| first=Judith A. | last=Irwin | year=2007
| title=Astrophysics: Decoding the Cosmos
| publisher=John Wiley and Sons | isbn=0-470-01306-0
| page=78 }}</ref> as measured by mass, with a small fraction of heavier elements. Typically the portion of heavy elements is measured in terms of the iron content of the stellar atmosphere, as iron is a common element and its absorption lines are relatively easy to measure. Because the molecular clouds where stars form are steadily enriched by heavier elements, a measurement of the chemical composition of a star can be used to infer its age.<ref>{{cite web
| date =2006-09-12 | url = http://www.eso.org/public/news/eso0634/
| title = A "Genetic Study" of the Galaxy
| publisher = ESO | accessdate = 2006-10-10 }}</ref>{{dubious|date=February 2014}} The portion of heavier elements may also be an indicator of the likelihood that the star has a planetary system.<ref>{{cite journal | last1=Fischer | first1=D. A.
| last2=Valenti | first2=J. | title=The Planet-Metallicity Correlation
| journal=The Astrophysical Journal | year=2005 | volume=622 | issue=2
| pages=1102–1117 | bibcode=2005ApJ...622.1102F | doi = 10.1086/428383 }}</ref>
 
The star with the lowest iron content ever measured is the dwarf HE1327-2326, with only 1/200,000th the iron content of the Sun.<ref>{{cite web
| date=April 17, 2005 | url=http://www.sciencedaily.com/releases/2005/04/050417162354.htm | title=Signatures Of The First Stars
| publisher=ScienceDaily | accessdate=2006-10-10 }}</ref> By contrast, the super-metal-rich star [[Mu Leonis|&mu; Leonis]] has nearly double the abundance of iron as the Sun, while the planet-bearing star [[14 Herculis]] has nearly triple the iron.<ref>{{cite journal
| last=Feltzing | first=S. | last2=Gonzalez | first2=G.
| title=The nature of super-metal-rich stars: Detailed abundance analysis of 8 super-metal-rich star candidates
| journal=Astronomy & Astrophysics
| year=2000 | volume=367 | issue=1 | pages=253–265
| bibcode=2001A&A...367..253F
| doi=10.1051/0004-6361:20000477 }}</ref> There also exist chemically [[peculiar star]]s that show unusual abundances of certain elements in their spectrum; especially [[chromium]] and [[rare earth element]]s.<ref>{{cite book
| first=David F. | last=Gray | year=1992
| title=The Observation and Analysis of Stellar Photospheres | pages=413–414
| publisher=Cambridge University Press
| isbn=0-521-40868-7 }}</ref>
 
===Diameter===
[[File:Star-sizes.jpg|left|thumb|Stars vary widely in size. In each image in the sequence, the right-most object appears as the left-most object in the next panel. The Earth appears at right in panel 1 and the Sun is second from the right in panel 3.]]
Due to their great distance from the Earth, all stars except the Sun appear to the unaided eye as shining points in the night sky that [[Scintillation (astronomy)|twinkle]] because of the effect of the Earth's atmosphere. The Sun is also a star, but it is close enough to the Earth to appear as a disk instead, and to provide daylight. Other than the Sun, the star with the largest apparent size is [[R Doradus]], with an [[angular diameter]] of only 0.057 [[arcsecond]]s.<ref>{{cite news
| title=The Biggest Star in the Sky | publisher=ESO
| date=March 11, 1997 | url=http://www.eso.org/public/news/eso9706/
| accessdate=2006-07-10 }}</ref>
 
The disks of most stars are much too small in [[angular size]] to be observed with current ground-based optical telescopes, and so [[interferometer]] telescopes are required to produce images of these objects. Another technique for measuring the angular size of stars is through [[occultation]]. By precisely measuring the drop in brightness of a star as it is occulted by the [[Moon]] (or the rise in brightness when it reappears), the star's angular diameter can be computed.<ref>{{cite journal
| last1=Ragland | first1=S. | last2=Chandrasekhar | first2=T.
| last3=Ashok | first3=N. M.
| title=Angular Diameter of Carbon Star Tx-Piscium from Lunar Occultation Observations in the Near Infrared
| journal=Journal of Astrophysics and Astronomy
| year=1995 | volume=16 | page=332
| bibcode=1995JApAS..16..332R }}</ref>
 
Stars range in size from [[neutron stars]], which vary anywhere from 20 to {{convert|40|km|0|abbr=on}} in diameter, to [[supergiant]]s like [[Betelgeuse]] in the [[Orion constellation]], which has a diameter approximately 650 times that of the Sun—about {{Convert|900000000|km|0|abbr=on|sigfig=2}}. Betelgeuse, however, has a much lower [[density]] than the Sun.<ref>{{cite web
| last=Davis | first=Kate | date=December 1, 2000
| url=http://www.aavso.org/vstar/vsots/1200.shtml
| title=Variable Star of the Month—December, 2000: Alpha Orionis
| publisher=AAVSO | accessdate=2006-08-13 | archiveurl=http://web.archive.org/web/20060712000904/http://www.aavso.org/vstar/vsots/1200.shtml <!-- Bot retrieved archive --> | archivedate=2006-07-12 }}</ref>
 
===Kinematics===
{{Main|Stellar kinematics}}
[[File:Pleiades large.jpg|thumb|right|300px|The [[Pleiades]], an [[open cluster]] of stars in the [[constellation]] of [[Taurus (constellation)|Taurus]]. These stars share a common motion through space.<ref>{{cite journal
| last=Loktin | first=A. V.
| title=Kinematics of stars in the Pleiades open cluster
| journal=Astronomy Reports | volume=50 | issue=9
| pages=714–721 |date=September 2006
| doi=10.1134/S1063772906090058 | bibcode=2006ARep...50..714L }}</ref> ''[[NASA]] photo'']]
The motion of a star relative to the Sun can provide useful information about the origin and age of a star, as well as the structure and evolution of the surrounding galaxy. The components of motion of a star consist of the [[radial velocity]] toward or away from the Sun, and the traverse angular movement, which is called its [[proper motion]].
 
Radial velocity is measured by the [[doppler shift]] of the star's spectral lines, and is given in units of [[kilometre|km]]/[[second|s]]. The proper motion of a star is determined by precise astrometric measurements in units of milli-[[arc second]]s (mas) per year. By determining the parallax of a star, the proper motion can then be converted into units of velocity. Stars with high rates of proper motion are likely to be relatively close to the Sun, making them good candidates for parallax measurements.<ref>{{cite web
| date=September 10, 1999 | url=http://www.rssd.esa.int/index.php?project=HIPPARCOS
| title=Hipparcos: High Proper Motion Stars
| publisher=ESA | accessdate=2006-10-10 }}</ref>
 
Once both rates of movement are known, the [[space velocity (astronomy)|space velocity]] of the star relative to the Sun or the galaxy can be computed. Among nearby stars, it has been found that younger population I stars have generally lower velocities than older, population II stars. The latter have elliptical orbits that are inclined to the plane of the galaxy.<ref>{{cite journal
| last = Johnson | first = Hugh M.
| title=The Kinematics and Evolution of Population I Stars
| journal=Publications of the Astronomical Society of the Pacific | year=1957 | volume=69 | issue=406 | page=54
| bibcode=1957PASP...69...54J
| doi=10.1086/127012 }}</ref> A comparison of the kinematics of nearby stars has also led to the identification of [[stellar association]]s. These are most likely groups of stars that share a common point of origin in giant molecular clouds.<ref>{{cite journal
| last1=Elmegreen | first1=B. | last2=Efremov | first2=Y. N.
| title=The Formation of Star Clusters
| journal=American Scientist
| year=1999 | volume=86 | issue=3 | page=264 | url=http://www.americanscientist.org/template/AssetDetail/assetid/15714/page/1
| accessdate=2006-08-23 | doi=10.1511/1998.3.264 | archiveurl = http://web.archive.org/web/20050323072521/http://www.americanscientist.org/template/AssetDetail/assetid/15714/page/1| archivedate = March 23, 2005|bibcode = 1998AmSci..86..264E }}</ref>
 
===Magnetic field===
{{Main|Stellar magnetic field}}
 
[[File:suaur.jpg|thumb|220px|Surface magnetic field of [[SU Aurigae|SU&nbsp;Aur]] (a young star of [[T Tauri star|T Tauri type]]), reconstructed by means of [[Zeeman-Doppler imaging]]]]
 
The [[magnetic field]] of a star is generated within regions of the interior where [[convection|convective]] circulation occurs. This movement of conductive plasma functions like a [[dynamo theory|dynamo]], generating magnetic fields that extend throughout the star. The strength of the magnetic field varies with the mass and composition of the star, and the amount of magnetic surface activity depends upon the star's rate of rotation. This surface activity produces [[starspot]]s, which are regions of strong magnetic fields and lower than normal surface temperatures. [[Coronal loop]]s are arching magnetic fields that reach out into the corona from active regions. [[Stellar flare]]s are bursts of high-energy particles that are emitted due to the same magnetic activity.<ref>{{cite web
| last=Brainerd | first=Jerome James
| date=July 6, 2005 | url=http://www.astrophysicsspectator.com/topics/observation/XRayCorona.html
| title=X-rays from Stellar Coronas
| publisher=The Astrophysics Spectator
| accessdate= 2007-06-21 }}</ref>
 
Young, rapidly rotating stars tend to have high levels of surface activity because of their magnetic field. The magnetic field can act upon a star's stellar wind, functioning as a brake to gradually slow the rate of rotation with time. Thus, older stars such as the Sun have a much slower rate of rotation and a lower level of surface activity. The activity levels of slowly rotating stars tend to vary in a cyclical manner and can shut down altogether for periods of time.<ref>{{cite web
| last = Berdyugina | first = Svetlana V. | year=2005
| url =http://solarphysics.livingreviews.org/Articles/lrsp-2005-8/
| title =Starspots: A Key to the Stellar Dynamo
| publisher =Living Reviews
| accessdate = 2007-06-21 }}</ref> During
the [[Maunder minimum]], for example, the Sun underwent a
70-year period with almost no sunspot activity.
 
===Mass===
{{Main|Stellar mass}}
One of the most massive stars known is [[Eta Carinae]],<ref>{{cite journal | first = Nathan | last = Smith | year = 1998 | url = http://www.astrosociety.org/pubs/mercury/9804/eta.html | title = The Behemoth Eta Carinae: A Repeat Offender | publisher = Astronomical Society of the Pacific | journal=Mercury Magazine | volume=27 | page=20 | accessdate = 2006-08-13 }}</ref> which, with 100–150&nbsp;times as much mass as the Sun, will have a lifespan of only several million years. A study of the [[Arches cluster]] suggests that 150&nbsp;solar masses is the upper limit for stars in the current era of the universe.<ref>{{cite news
| title=NASA's Hubble Weighs in on the Heaviest Stars in the Galaxy
| publisher=NASA News | date=March 3, 2005 | url=http://www.nasa.gov/home/hqnews/2005/mar/HQ_05071_HST_galaxy.html
| accessdate=2006-08-04 }}</ref> The reason for this limit is not precisely known, but it is partially due to the [[Eddington luminosity]] which defines the maximum amount of luminosity that can pass through the atmosphere of a star without ejecting the gases into space. However, a star named [[R136a1]] in the Large Magellanic Cloud, RMC 136a star cluster has been measured at 265 solar masses, which puts this limit into question.<ref name=eso20100721>{{cite news
| title=Stars Just Got Bigger
| publisher=European Southern Observatory
| date=July 21, 2010
| url=http://www.eso.org/public/news/eso1030/
| accessdate=2010-17-24 }}</ref> A study determined that stars larger than 150 solar masses in [[R136]] were created through the collision and merger of massive stars in close [[binary star|binary systems]], providing a way to sidestep the 150 solar mass limit.<ref>{{cite web | work=LiveScience.com | url=http://news.yahoo.com/mystery-monster-stars-solved-monster-mash-161251348.html?_esi=1 | title=Mystery of the 'Monster Stars' Solved: It Was a Monster Mash | first1=Natalie | last1=Wolchover | date=August 7, 2012 }}</ref>
 
[[File:Ngc1999.jpg|thumb|right|250px|The [[reflection nebula]] [[NGC 1999]] is brilliantly illuminated by V380 Orionis (center), a variable star with about 3.5&nbsp;times the mass of the Sun. The black patch of sky is a vast hole of empty space and not a [[dark nebula]] as previously thought. ''NASA image'']]
 
The first stars to form after the Big Bang may have been larger, up to 300 solar masses or more,<ref>{{cite news
| title=Ferreting Out The First Stars
| publisher=Harvard-Smithsonian Center for Astrophysics
| date=September 22, 2005 | url=http://www.cfa.harvard.edu/news/2005/pr200531.html
| accessdate=2006-09-05 }}</ref> due to the complete absence of elements heavier than [[lithium]] in their composition. This generation of supermassive, [[population III stars]] is long extinct, however, and currently only theoretical.
 
With a mass only 93&nbsp;times that of [[Jupiter]], [[AB Doradus|AB Doradus C]], a companion to AB Doradus A, is the smallest known star undergoing nuclear fusion in its core.<ref>{{cite news
| title=Weighing the Smallest Stars | publisher=ESO
| date=January 1, 2005 | url=http://www.eso.org/public/news/eso0503/
| accessdate=2006-08-13 }}</ref> For stars with similar metallicity to the Sun, the theoretical minimum mass the star can have, and still undergo fusion at the core, is estimated to be about 75 times the mass of Jupiter.<ref>{{cite web
| first=Alan | last=Boss | date=April 3, 2001
| url=http://www.carnegieinstitution.org/News4-3,2001.html
| title=Are They Planets or What?
| publisher=Carnegie Institution of Washington
| accessdate=2006-06-08 | archiveurl=http://web.archive.org/web/20060928065124/http://www.carnegieinstitution.org/News4-3,2001.html <!-- Bot retrieved archive --> | archivedate =2006-09-28 }}</ref><ref name="minimum">{{cite web | last=Shiga | first=David
| date=August 17, 2006 | url=http://www.newscientistspace.com/article/dn9771-mass-cutoff-between-stars-and-brown-dwarfs-revealed.html | archiveurl=http://web.archive.org/web/20061114221813/space.newscientist.com/article/dn9771-mass-cutoff-between-stars-and-brown-dwarfs-revealed.html | archivedate=2006-11-14
| title=Mass cut-off between stars and brown dwarfs revealed
| publisher=New Scientist
| accessdate=2006-08-23 }}</ref> When the metallicity is very low, however, a recent study of the faintest stars found that the minimum star size seems to be about 8.3% of the solar mass, or about 87 times the mass of Jupiter.<ref name="minimum" /><ref>{{cite news
| title=Hubble glimpses faintest stars
| publisher=BBC | date=August 18, 2006
| url=http://news.bbc.co.uk/2/hi/science/nature/5260008.stm
| accessdate=2006-08-22
| first=Elli
| last=Leadbeater}}</ref> Smaller bodies are called [[brown dwarf]]s, which occupy a poorly defined grey area between stars and [[gas giant]]s.
 
The combination of the radius and the mass of a star determines the surface gravity. Giant stars have a much lower surface gravity than main sequence stars, while the opposite is the case for degenerate, compact stars such as white dwarfs. The surface gravity can influence the appearance of a star's spectrum, with higher gravity causing a broadening of the [[absorption line]]s.<ref name="new cosmos" />
 
===Rotation===
{{Main|Stellar rotation}}
 
The rotation rate of stars can be determined through [[spectroscopy|spectroscopic measurement]], or more exactly determined by tracking the rotation rate of [[starspot]]s. Young stars can have a rapid rate of rotation greater than 100&nbsp;km/s at the equator. The B-class star [[Achernar]], for example, has an equatorial rotation velocity of about 225&nbsp;km/s or greater, causing its equator to be slung outward and giving it an equatorial diameter that is more than 50% larger than the distance between the poles. This rate of rotation is just below the critical velocity of 300&nbsp;km/s where the star would break apart.<ref>{{cite news
| title=Flattest Star Ever Seen | publisher=ESO
| date=June 11, 2003 | url=http://www.eso.org/public/news/eso0316/
| accessdate=2006-10-03 }}</ref> By contrast, the Sun only rotates once every 25 – 35 days, with an equatorial velocity of 1.994&nbsp;km/s. The star's magnetic field and the stellar wind serve to slow a [[main sequence star|main sequence star's]] rate of rotation by a significant amount as it evolves on the main sequence.<ref>{{cite web
| last=Fitzpatrick | first=Richard
| date=February 13, 2006 | url=http://farside.ph.utexas.edu/teaching/plasma/lectures/lectures.html
| archiveurl=http://web.archive.org/web/20100104142353/http://farside.ph.utexas.edu/teaching/plasma/lectures/lectures.html
| archivedate=2010-01-04
| title=Introduction to Plasma Physics: A graduate course
| publisher=The University of Texas at Austin
| accessdate=2006-10-04 }}</ref>
 
[[Degenerate star]]s have contracted into a compact mass, resulting in a rapid rate of rotation. However they have relatively low rates of rotation compared to what would be expected by conservation of [[angular momentum]]—the tendency of a rotating body to compensate for a contraction in size by increasing its rate of spin. A large portion of the star's angular momentum is dissipated as a result of mass loss through the stellar wind.<ref>{{cite journal | last = Villata | first = Massimo | title=Angular momentum loss by a stellar wind and rotational velocities of white dwarfs | journal=Monthly Notices of the Royal Astronomical Society | year=1992 | volume=257 | issue=3 | pages=450–454 | bibcode=1992MNRAS.257..450V }}</ref> In spite of this, the rate of rotation for a pulsar can be very rapid. The pulsar at the heart of the [[Crab nebula]], for example, rotates 30 times per second.<ref>{{cite news
| title=A History of the Crab Nebula | publisher=ESO
| date=May 30, 1996 | url=http://hubblesite.org/newscenter/archive/releases/1996/22/astrofile/
| accessdate=2006-10-03 }}</ref> The rotation rate of the pulsar will gradually slow due to the emission of radiation.
 
===Temperature===
 
The surface temperature of a main sequence star is determined by the rate of energy production at the core and by its radius, and is often estimated from the star's [[color index]].<ref name="astronomynotes">{{cite web
|url=http://www.astronomynotes.com/starprop/s5.htm
|title=Properties of Stars: Color and Temperature
|accessdate=2007-10-09 |last=Strobel |first=Nick
|date=August 20, 2007 |work=Astronomy Notes
|publisher=Primis/McGraw-Hill, Inc.
|archiveurl=http://web.archive.org/web/20070626090138/http://www.astronomynotes.com/starprop/s5.htm
|archivedate=2007-06-26 }}</ref> The temperature is normally given as the [[effective temperature]], which is the temperature of an idealized [[black body]] that radiates its energy at the same luminosity per surface area as the star. Note that the effective temperature is only a representative value, as the temperature increases toward the core.<ref>{{cite web
| first=Courtney | last=Seligman | work=Self-published
| url=http://cseligman.com/text/stars/heatflowreview.htm
| title =Review of Heat Flow Inside Stars
| accessdate = 2007-07-05 }}</ref> The temperature in the core region of a star is several million&nbsp;[[kelvin]]s.<ref name="aps_mss" />
 
The stellar temperature will determine the rate of ionization of various elements, resulting in characteristic absorption lines in the spectrum. The surface temperature of a star, along with its visual [[absolute magnitude]] and absorption features, is used to classify a star (see classification below).<ref name="new cosmos" />
 
Massive main sequence stars can have surface temperatures of 50,000&nbsp;[[Kelvin|K]]. Smaller stars such as the Sun have surface temperatures of a few thousand [[Kelvin|K]]. Red giants have relatively low surface temperatures of about 3,600&nbsp;K; but they also have a high luminosity due to their large exterior surface area.<ref name=zeilik>{{cite book | last1=Zeilik | first1=Michael A. | last2=Gregory | first2=Stephan A. | title=Introductory Astronomy & Astrophysics | edition=4th | year=1998 | publisher=Saunders College Publishing | isbn=0-03-006228-4 | page=321 }}</ref>
 
==Radiation==
The energy produced by stars, as a product of nuclear fusion, radiates into space as both [[electromagnetic radiation]] and [[particle radiation]]. The particle radiation emitted by a star is manifested as the stellar wind,<ref>{{cite news
| last=Koppes | first=Steve
| title=University of Chicago physicist receives Kyoto Prize for lifetime achievements in science
| publisher=The University of Chicago News Office
| date=June 20, 2003 | url=http://www-news.uchicago.edu/releases/03/030620.parker.shtml
| accessdate=2012-06-15 }}</ref> which streams from the outer layers as free [[proton]]s, and electrically charged [[alpha particle|alpha]], and [[beta particle]]s. Although almost massless there also exists a steady stream of [[neutrino]]s emanating from the star's core.
 
The production of energy at the core is the reason stars shine so brightly: every time two or more atomic nuclei fuse together to form a single [[atomic nucleus]] of a new heavier element, [[gamma ray]] [[photon]]s are released from the nuclear fusion product. This energy is converted to other forms of [[electromagnetic energy]] of lower frequency, such as visible light, by the time it reaches the star's outer layers.
 
The [[color]] of a star, as determined by the most intense [[frequency]] of the visible light, depends on the temperature of the star's outer layers, including its [[photosphere]].<ref>{{cite web | url = http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html | title = The Colour of Stars | publisher = Australian Telescope Outreach and Education | accessdate = 2006-08-13 }}</ref> Besides visible light, stars also emit forms of electromagnetic radiation that are invisible to the [[human eye]]. In fact, stellar electromagnetic radiation spans the entire [[electromagnetic spectrum]], from the longest [[wavelength]]s of [[radio frequency|radio wave]]s through [[infrared]], visible light, [[ultraviolet]], to the shortest of [[X-ray]]s, and [[gamma rays]]. From the standpoint of total energy emitted by a star, not all components of stellar electromagnetic radiation are significant, but all frequencies provide insight into the star's physics.
 
Using the [[Astronomical spectroscopy|stellar spectrum]], astronomers can also determine the surface temperature, [[surface gravity]], metallicity and [[rotation]]al velocity of a star. If the distance of the star is known, such as by measuring the parallax, then the luminosity of the star can be derived. The mass, radius, surface gravity, and rotation period can then be estimated based on stellar models. (Mass can be calculated for stars in [[binary system (astronomy)|binary systems]] by measuring their orbital velocities and distances. [[Gravitational microlensing]] has been used to measure the mass of a single star.<ref>{{cite news
| title=Astronomers Measure Mass of a Single Star—First Since the Sun
| publisher=Hubble News Desk | date=July 15, 2004 | url=http://hubblesite.org/newscenter/archive/releases/2004/24/text/
| accessdate=2006-05-24 }}</ref>) With these parameters, astronomers can also estimate the age of the star.<ref>{{cite journal
| last1=Garnett | first1=D. R. | last2=Kobulnicky | first2=H. A.
| title=Distance Dependence in the Solar Neighborhood Age-Metallicity Relation
| journal=The Astrophysical Journal | year=2000
| volume=532
| issue= 2 | pages=1192–1196
| doi = 10.1086/308617
| bibcode=2000ApJ...532.1192G|arxiv = astro-ph/9912031 }}</ref>
 
===Luminosity===
 
The luminosity of a star is the amount of [[light]] and other forms of [[radiant energy]] it radiates per unit of time. It has units of [[power (physics)|power]]. The luminosity of a star is determined by the radius and the surface temperature. However, many stars do not radiate a uniform [[flux]] (the amount of energy radiated per unit area) across their entire surface. The rapidly rotating star [[Vega]], for example, has a higher energy flux at its poles than along its equator.<ref>{{cite news
| author=Staff | date=January 10, 2006
| title=Rapidly Spinning Star Vega has Cool Dark Equator
| publisher=National Optical Astronomy Observatory
| url=http://www.noao.edu/outreach/press/pr06/pr0603.html
| accessdate=2007-11-18
}}</ref>
 
Surface patches with a lower temperature and luminosity than average are known as [[sunspot|starspots]]. Small, ''dwarf'' stars such as our Sun generally have essentially featureless disks with only small starspots. Larger, ''giant'' stars have much larger, more obvious starspots,<ref name="Michelson Starspots">{{cite journal | last1=Michelson | first1=A. A. | last2=Pease | first2=F. G. | title=Starspots: A Key to the Stellar Dynamo | journal=Living Reviews in Solar Physics | publisher=Max Planck Society | year=2005 | url=http://solarphysics.livingreviews.org/Articles/lrsp-2005-8/ }}</ref> and they also exhibit strong stellar [[limb darkening]]. That is, the brightness decreases towards the edge of the stellar disk.<ref>{{cite journal | last1=Manduca | first1=A. | last2=Bell | first2=R. A. | last3=Gustafsson | first3=B. | title=Limb darkening coefficients for late-type giant model atmospheres | journal=Astronomy and Astrophysics | year=1977 | volume=61 | issue=6 | pages=809–813 | bibcode=1977A&A....61..809M }}</ref> Red dwarf [[flare star]]s such as [[UV Ceti]] may also possess prominent starspot features.<ref>{{cite journal | last1=Chugainov | first1=P. F. | title=On the Cause of Periodic Light Variations of Some Red Dwarf Stars | journal=Information Bulletin on Variable Stars | year=1971 | volume=520 | pages=1–3 | bibcode=1971IBVS..520....1C }}</ref>
 
===Magnitude===
{{Main|Apparent magnitude|Absolute magnitude}}
 
The apparent [[brightness]] of a star is expressed in terms of its [[apparent magnitude]], which is the brightness of a star and is a function of the star's luminosity, distance from Earth, and the altering of the star's light as it passes through Earth's atmosphere. Intrinsic or absolute magnitude is directly related to a star's luminosity and is what the apparent magnitude a star would be if the distance between the Earth and the star were 10 parsecs (32.6 light-years).
 
{| class="wikitable" style="float: right; margin-left: 1em;"
|+ ''Number of stars brighter than magnitude''
!Apparent<br />magnitude
!Number&nbsp;<br />of&nbsp;Stars<ref>{{cite web | url = http://www.nso.edu/PR/answerbook/magnitude.html | archiveurl = http://web.archive.org/web/20080206074842/http://www.nso.edu/PR/answerbook/magnitude.html | archivedate = 2008-02-06 | title = Magnitude | publisher = National Solar Observatory—Sacramento Peak | accessdate = 2006-08-23 }}</ref>
|- style="text-align: center;"
||0
||4
|- style="text-align: center;"
||1
||15
|- style="text-align: center;"
||2
||48
|- style="text-align: center;"
||3
||171
|- style="text-align: center;"
||4
||513
|- style="text-align: center;"
||5
||1,602
|- style="text-align: center;"
||6
||4,800
|- style="text-align: center;"
||7
||14,000
|}
 
Both the apparent and absolute magnitude scales are [[logarithmic units]]: one whole number difference in magnitude is equal to a brightness variation of about 2.5 times<ref name="luminosity">{{cite web | url = http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_luminosity.html | title = Luminosity of Stars | publisher = Australian Telescope Outreach and Education | accessdate = 2006-08-13 }}</ref> (the [[nth root|5th root]] of 100 or approximately 2.512). This means that a first magnitude (+1.00) star is about 2.5 times brighter than a second magnitude (+2.00) star, and approximately 100 times brighter than a sixth magnitude (+6.00) star. The faintest stars visible to the naked eye under good seeing conditions are about magnitude +6.
 
On both apparent and absolute magnitude scales, the smaller the magnitude number, the brighter the star; the larger the magnitude number, the fainter. The brightest stars, on either scale, have negative magnitude numbers. The variation in brightness (Δ''L'') between two stars is calculated by subtracting the magnitude number of the brighter star (''m''<sub>b</sub>) from the magnitude number of the fainter star (''m''<sub>f</sub>), then using the difference as an exponent for the base number 2.512; that is to say:
 
:<math> \Delta{m} = m_\mathrm{f} - m_\mathrm{b} </math>
:<math>2.512^{\Delta{m}} = \Delta{L}</math>
 
Relative to both luminosity and distance from Earth, a star's absolute magnitude (''M'') and apparent magnitude (''m'') are not equivalent;<ref name="luminosity" /> for example, the bright star Sirius has an apparent magnitude of −1.44, but it has an absolute magnitude of +1.41.
 
The Sun has an apparent magnitude of −26.7, but its absolute magnitude is only +4.83. Sirius, the brightest star in the night sky as seen from Earth, is approximately 23 times more luminous than the Sun, while [[Canopus]], the second brightest star in the night sky with an absolute magnitude of −5.53, is approximately 14,000 times more luminous than the Sun. Despite Canopus being vastly more luminous than Sirius, however, Sirius appears brighter than Canopus. This is because Sirius is merely 8.6 light-years from the Earth, while Canopus is much farther away at a distance of 310 light-years.
 
As of 2006, the star with the highest known absolute magnitude is [[LBV 1806-20]], with a magnitude of −14.2. This star is at least 5,000,000 times more luminous than the Sun.<ref>{{cite web
| last1=Hoover | first1=Aaron | date =January 15, 2004
| url=http://www.napa.ufl.edu/2004news/bigbrightstar.htm
| archiveurl=http://web.archive.org/web/20070807035239/http://www.napa.ufl.edu/2004news/bigbrightstar.htm
| archivedate=2007-08-07
| title=Star may be biggest, brightest yet observed
| publisher=HubbleSite | accessdate=2006-06-08 }}</ref> The least luminous stars that are currently known are located in the [[NGC 6397]] cluster. The faintest red dwarfs in the cluster were magnitude 26, while a 28th magnitude white dwarf was also discovered. These faint stars are so dim that their light is as bright as a birthday candle on the Moon when viewed from the Earth.<ref>{{cite web
| date=August 17, 2006 | url=http://hubblesite.org/newscenter/archive/releases/2006/37/image/a/
| title=Faintest Stars in Globular Cluster NGC 6397
| publisher=HubbleSite | accessdate=2006-06-08 }}</ref>
 
==Classification==
{| class="wikitable" style="float: right; text-align: center; margin-left: 1em;"
|+ ''Surface Temperature Ranges for<br />Different Stellar Classes''<ref>{{cite web
| last=Smith | first=Gene | date=April 16, 1999
| url=http://casswww.ucsd.edu/public/tutorial/Stars.html
| title=Stellar Spectra
| publisher=University of California, San Diego
| accessdate=2006-10-12 }}</ref>
! Class
! Temperature
! Sample star
|- style="background: {{star-color|O}}"
| O
| 33,000&nbsp;K&nbsp;or&nbsp;more
| [[Zeta Ophiuchi]]
|- style="background: {{star-color|B}}"
| B
| 10,500–30,000&nbsp;K
| [[Rigel]]
|- style="background: {{star-color|A}}"
| A
| 7,500–10,000&nbsp;K
| [[Altair]]
|- style="background: {{star-color|F}}"
| F
| 6,000–7,200&nbsp;K
| [[Procyon|Procyon&nbsp;A]]
|- style="background: {{star-color|G}}"
| G
| 5,500–6,000&nbsp;K
| [[Sun]]
|- style="background: {{star-color|K}}"
| K
| 4,000–5,250&nbsp;K
| [[Epsilon Indi]]
|- style="background: {{star-color|M}}"
| M
| 2,600–3,850&nbsp;K
| [[Proxima Centauri]]
|}
{{Main|Stellar classification}}
 
The current stellar classification system originated in the early 20th century, when stars were classified from ''A'' to ''Q'' based on the strength of the [[hydrogen line]].<ref>{{cite journal
| last=Fowler | first=A.
| title=The Draper Catalogue of Stellar Spectra
| journal=Nature
| year=1891–2 | volume=45 | pages=427–8 | doi = 10.1038/045427a0 |bibcode = 1892Natur..45..427F }}</ref> It was not known at the time that the major influence on the line strength was temperature; the hydrogen line strength reaches a peak at over 9000&nbsp;K, and is weaker at both hotter and cooler temperatures. When the classifications were reordered by temperature, it more closely resembled the modern scheme.<ref name=carlos>{{cite book
| first1=Carlos | last1=Jaschek | last2=Jaschek | first2=Mercedes
| year=1990 | title=The Classification of Stars
| publisher=Cambridge University Press | pages=31–48
| isbn=0-521-38996-8 }}</ref>
 
Stars are given a single-letter classification according to their spectra, ranging from type ''O'', which are very hot, to ''M'', which are so cool that molecules may form in their atmospheres. The main classifications in order of decreasing surface temperature are: ''O, B, A, F, G, K'', and ''M''. A variety of rare spectral types have special classifications. The most common of these are types ''L'' and ''T'', which classify the coldest low-mass stars and brown dwarfs. Each letter has 10 sub-divisions, numbered from 0 to 9, in order of decreasing temperature. However, this system breaks down at extreme high temperatures: class ''O0'' and ''O1'' stars may not exist.<ref name="spectrum">{{cite web
| first=Alan M | last=MacRobert
| url =http://www.skyandtelescope.com/howto/basics/3305876.html
| title = The Spectral Types of Stars
| publisher = Sky and Telescope
| accessdate = 2006-07-19 }}</ref>
 
In addition, stars may be classified by the luminosity effects found in their spectral lines, which correspond to their spatial size and is determined by the surface gravity. These range from ''0'' ([[hypergiant]]s) through ''III'' ([[giant star|giant]]s) to ''V'' (main sequence dwarfs); some authors add ''VII'' (white dwarfs). Most stars belong to the [[main sequence]], which consists of ordinary [[hydrogen burning process|hydrogen-burning]] stars. These fall along a narrow, diagonal band when graphed according to their absolute magnitude and spectral type.<ref name="spectrum" /> The Sun is a main sequence ''G2V'' yellow dwarf of intermediate temperature and ordinary size.
 
Additional nomenclature, in the form of lower-case letters, can follow the spectral type to indicate peculiar features of the spectrum. For example, an "''e''" can indicate the presence of emission lines; "''m''" represents unusually strong levels of metals, and "''var''" can mean variations in the spectral type.<ref name="spectrum" />
 
White dwarf stars have their own class that begins with the letter ''D''. This is further sub-divided into the classes ''DA'', ''DB'', ''DC'', ''DO'', ''DZ'', and ''DQ'', depending on the types of prominent lines found in the spectrum. This is followed by a numerical value that indicates the temperature index.<ref>{{cite web
| url = http://www.physics.uq.edu.au/people/ross/ph3080/whitey.htm
| archiveurl = http://web.archive.org/web/20091008115925/http://www.physics.uq.edu.au/people/ross/ph3080/whitey.htm
| archivedate = 2009-10-08
| title = White Dwarf (wd) Stars
| publisher = White Dwarf Research Corporation
| accessdate = 2006-07-19 }}</ref>
 
==Variable stars==
{{Main|Variable star}}
[[File:Mira 1997.jpg|right|thumb|200px|The asymmetrical appearance of [[Mira]], an oscillating variable star. ''NASA [[Hubble Space Telescope|HST]] image'']]
Variable stars have periodic or random changes in luminosity because of intrinsic or extrinsic properties. Of the intrinsically variable stars, the primary types can be subdivided into three principal groups.
 
During their stellar evolution, some stars pass through phases where they can become pulsating variables. Pulsating variable stars vary in radius and luminosity over time, expanding and contracting with periods ranging from minutes to years, depending on the size of the star. This category includes [[Cepheid variable|Cepheid and cepheid-like stars]], and long-period variables such as [[Mira variable|Mira]].<ref name="variables">{{cite web | url=http://www.aavso.org/types-variables | title=Types of Variable | date=May 11, 2010 | publisher=AAVSO | accessdate=2010-08-20 }}</ref>
 
Eruptive variables are stars that experience sudden increases in luminosity because of flares or mass ejection events.<ref name="variables" /> This group includes protostars, Wolf-Rayet stars, and [[Flare star]]s, as well as giant and supergiant stars.
 
Cataclysmic or explosive variable stars are those that undergo a dramatic change in their properties. This group includes [[nova]]e and supernovae. A binary star system that includes a nearby white dwarf can produce certain types of these spectacular stellar explosions, including the nova and a Type 1a supernova.<ref name="iben" /> The explosion is created when the white dwarf accretes hydrogen from the companion star, building up mass until the hydrogen undergoes fusion.<ref>{{cite web
| date =2004-11-01 | url = http://imagine.gsfc.nasa.gov/docs/science/know_l2/cataclysmic_variables.html
| title = Cataclysmic Variables
| publisher = NASA Goddard Space Flight Center
| accessdate = 2006-06-08 }}</ref> Some novae are also recurrent, having periodic outbursts of moderate amplitude.<ref name="variables" />
 
Stars can also vary in luminosity because of extrinsic factors, such as eclipsing binaries, as well as rotating stars that produce extreme starspots.<ref name="variables" /> A notable example of an eclipsing binary is Algol, which regularly varies in magnitude from 2.3 to 3.5 over a period of 2.87 days.
 
==Structure==
{{Main|Stellar structure}}
[[Image:Star types.svg|350px|left|thumb|Internal structures of [[main sequence stars]], convection zones with arrowed cycles and radiative zones with red flashes. To the left a '''low-mass''' [[red dwarf]], in the center a '''mid-sized''' [[yellow dwarf]] and at the right a '''massive''' [[blue-white main sequence star]].]]
The interior of a stable star is in a state of [[hydrostatic equilibrium]]: the forces on any small volume almost exactly counterbalance each other. The balanced forces are inward gravitational force and an outward force due to the pressure [[gradient]] within the star. The [[pressure gradient]] is established by the temperature gradient of the plasma; the outer part of the star is cooler than the core. The temperature at the core of a main sequence or giant star is at least on the order of 10<sup>7</sup> [[kelvin|K]]. The resulting temperature and pressure at the hydrogen-burning core of a main sequence star are sufficient for [[nuclear fusion]] to occur and for sufficient energy to be produced to prevent further collapse of the star.<ref name="hansen">{{cite book | last1=Hansen | first1=Carl J. | last2=Kawaler | first2=Steven D. | last3=Trimble | first3=Virginia | pages=32–33 | title=Stellar Interiors | publisher=Springer | year=2004 | isbn=0-387-20089-4 }}</ref><ref name="Schwarzschild">{{cite book
| first=Martin | last=Schwarzschild | title=Structure and Evolution of the Stars | publisher=Princeton University Press | year=1958 | isbn=0-691-08044-5}}<!-- Book republished by Dover as ISBN 0-486-61479-4, but ISBN in the cite book template is the one as published by Prin. Univ. Press--></ref>
 
As atomic nuclei are fused in the core, they emit energy in the form of [[gamma ray]]s. These photons interact with the surrounding plasma, adding to the thermal energy at the core. Stars on the main sequence convert hydrogen into helium, creating a slowly but steadily increasing proportion of helium in the core. Eventually the helium content becomes predominant and energy production ceases at the core. Instead, for stars of more than 0.4 solar masses, fusion occurs in a slowly expanding shell around the [[degenerate matter|degenerate]] helium core.<ref>{{cite web | url = http://aether.lbl.gov/www/tour/elements/stellar/stellar_a.html | title = Formation of the High Mass Elements | publisher = Smoot Group | accessdate = 2006-07-11 }}</ref>
 
In addition to hydrostatic equilibrium, the interior of a stable star will also maintain an energy balance of [[thermal equilibrium]]. There is a radial temperature gradient throughout the interior that results in a flux of energy flowing toward the exterior. The outgoing flux of energy leaving any layer within the star will exactly match the incoming flux from below.
 
The [[radiation zone]] is the region within the stellar interior where radiative transfer is sufficiently efficient to maintain the flux of energy. In this region the plasma will not be perturbed and any mass motions will die out. If this is not the case, however, then the plasma becomes unstable and convection will occur, forming a [[convection zone]]. This can occur, for example, in regions where very high energy fluxes occur, such as near the core or in areas with high [[opacity (optics)|opacity]] as in the outer envelope.<ref name="Schwarzschild" />
 
The occurrence of convection in the outer envelope of a main sequence star depends on the mass. Stars with several times the mass of the Sun have a convection zone deep within the interior and a radiative zone in the outer layers. Smaller stars such as the Sun are just the opposite, with the convective zone located in the outer layers.<ref name="imagine">{{cite web | date =2006-09-01 | url = http://imagine.gsfc.nasa.gov/docs/science/know_l2/stars.html | title = What is a Star? | publisher = NASA | accessdate = 2006-07-11 }}</ref> Red dwarf stars with less than 0.4 solar masses are convective throughout, which prevents the accumulation of a helium core.<ref name="late stages" /> For most stars the convective zones will also vary over time as the star ages and the constitution of the interior is modified.<ref name="Schwarzschild" />
 
[[File:Sun parts big.jpg|thumb|360px|right|This diagram shows a cross-section of the [[Sun]]. ''NASA image'']]
The portion of a star that is visible to an observer is called the [[photosphere]]. This is the layer at which the plasma of the star becomes transparent to photons of light. From here, the energy generated at the core becomes free to propagate out into space. It is within the photosphere that [[sun spots]], or regions of lower than average temperature, appear.
 
Above the level of the photosphere is the [[stellar atmosphere]]. In a main sequence star such as the Sun, the lowest level of the atmosphere is the thin [[chromosphere]] region, where [[spicule (solar physics)|spicule]]s appear and [[Solar flare|stellar flares]] begin. This is surrounded by a transition region, where the temperature rapidly increases within a distance of only {{convert|100|km|0|abbr=on}}. Beyond this is the [[corona]], a volume of super-heated plasma that can extend outward to several million kilometres.<ref>{{cite press release
| publisher=ESO | date=August 1, 2001
| title=The Glory of a Nearby Star: Optical Light from a Hot Stellar Corona Detected with the VLT
| url=http://www.eso.org/public/news/eso0127/
| accessdate=2006-07-10 }}</ref> The existence of a corona appears to be dependent on a convective zone in the outer layers of the star.<ref name="imagine" /> Despite its high temperature, the corona emits very little light. The corona region of the Sun is normally only visible during a [[solar eclipse]].
 
From the corona, a [[stellar wind]] of plasma particles expands outward from the star, propagating until it interacts with the [[interstellar medium]]. For the Sun, the influence of its [[solar wind]] extends throughout the bubble-shaped region of the [[heliosphere]].<ref>{{cite journal | display-authors=1
| last1=Burlaga | first1=L. F. | last2=Ness | first2=N. F. | last3=Acuña | first3=M. H. | last4=Lepping | first4=R. P. | last5=Connerney | first5=J. E. P. | last6=Stone | first6=E. C. | last7=McDonald | first7=F. B.
| title=Crossing the Termination Shock into the Heliosheath: Magnetic Fields
| journal=Science | year=2005 | volume=309
| issue=5743 | pages=2027–2029 | doi= 10.1126/science.1117542
| pmid=16179471 | bibcode=2005Sci...309.2027B }}</ref>
 
==Nuclear fusion reaction pathways==
{{Main|Stellar nucleosynthesis}}
{{Multiple image|direction=vertical|align=right|image1=FusionintheSun.svg|image2=CNO Cycle.svg|width=200|caption1=Overview of the proton-proton chain|caption2=The carbon-nitrogen-oxygen cycle}}
A variety of different nuclear fusion reactions take place inside the cores of stars, depending upon their mass and composition, as part of [[stellar nucleosynthesis]]. The net mass of the fused atomic nuclei is smaller than the sum of the constituents. This lost mass is released as electromagnetic energy, according to the [[mass-energy equivalence]] relationship ''E''&nbsp;=&nbsp;''mc''<sup>2</sup>.<ref name="sunshine" />
 
The hydrogen fusion process is temperature-sensitive, so a moderate increase in the core temperature will result in a significant increase in the fusion rate. As a result the core temperature of main sequence stars only varies from 4 million kelvin for a small M-class star to 40 million kelvin for a massive O-class star.<ref name="aps_mss">{{cite web
| date=February 16, 2005 | url=http://www.astrophysicsspectator.com/topics/stars/MainSequence.html
| title=Main Sequence Stars
| publisher=The Astrophysics Spectator
| accessdate=2006-10-10 }}</ref>
 
In the Sun, with a 10-million-kelvin core, hydrogen fuses to form helium in the [[proton-proton chain reaction]]:<ref name="synthesis">{{cite journal | display-authors=1 | last1=Wallerstein | first1=G. | last2=Iben Jr. | first2=I. | last3=Parker | first3=P. | last4=Boesgaard | first4=A. M. | last5=Hale | first5=G. M. | last6=Champagne | first6=A. E. | last7=Barnes | first7=C. A. | last8=KM-dppeler | first8=F. | last9=Smith | first9=V. V. | last10=Hoffman | first10=R. D. | last11=Timmes | first11=F. X. | last12=Sneden | first12=C. | last13=Boyd | first13=R. N. | last14=Meyer | first14=B. S. | last15=Lambert | first15=D. L. | title=Synthesis of the elements in stars: forty years of progress | journal=Reviews of Modern Physics | year=1999 | volume=69 | issue=4 | pages=995–1084 | url=http://authors.library.caltech.edu/10255/1/WALrmp97.pdf| format=PDF | accessdate=2006-08-04 | doi=10.1103/RevModPhys.69.995 | bibcode=1997RvMP...69..995W}}</ref>
:4[[Hydrogen-1|<sup>1</sup>H]] → 2[[deuterium|<sup>2</sup>H]] + 2[[positron|e<sup>+</sup>]] + 2[[neutrino|ν<sub>e</sub>]] (4.0 M[[electronvolt|eV]] + 1.0 MeV)
:2<sup>1</sup>H + 2<sup>2</sup>H → 2[[Helium-3|<sup>3</sup>He]] + 2[[photon|γ]] (5.5 MeV)
:2<sup>3</sup>He → [[Helium-4|<sup>4</sup>He]] + 2<sup>1</sup>H (12.9 MeV)
 
These reactions result in the overall reaction:
 
:4<sup>1</sup>H → <sup>4</sup>He + 2e<sup>+</sup> + 2γ + 2ν<sub>e</sub> (26.7 MeV)
 
where e<sup>+</sup> is a [[positron]], γ is a gamma ray photon, ν<sub>e</sub> is a [[neutrino]], and H and He are isotopes of hydrogen and helium, respectively. The energy released by this reaction is in millions of electron volts, which is actually only a tiny amount of energy. However enormous numbers of these reactions occur constantly, producing all the energy necessary to sustain the star's radiation output.
 
{| class="wikitable" style="float: left; margin-right: 0.5em;"
|+ Minimum stellar mass required for fusion
|-
!Element
![[Solar mass|Solar<br />masses]]
|-
| Hydrogen ||style="text-align: center;"| 0.01
|-
| Helium ||style="text-align: center;"| 0.4
|-
| Carbon ||style="text-align: center;"| 5<ref>{{cite journal
| last1=Girardi | first1=L. | last2=Bressan | first2=A. | last3=Bertelli | first3=G. | last4=Chiosi | first4=C. | title=Evolutionary tracks and isochrones for low- and intermediate-mass stars: From 0.15 to 7 M<sub>sun</sub>, and from Z=0.0004 to 0.03
| journal=Astronomy and Astrophysics Supplement
| year=2000 | volume=141
| issue=3 | pages=371–383
| doi=10.1051/aas:2000126 |arxiv = astro-ph/9910164 |bibcode = 2000A&AS..141..371G }}</ref>
|-
| Neon ||style="text-align: center;"| 8
|}
In more massive stars, helium is produced in a cycle of reactions [[catalyst|catalyzed]] by carbon—the [[CNO cycle|carbon-nitrogen-oxygen cycle]].<ref name="synthesis" />
 
In evolved stars with cores at 100 million kelvin and masses between 0.5 and 10 solar masses, helium can be transformed into carbon in the [[triple-alpha process]] that uses the intermediate element [[beryllium]]:<ref name="synthesis" />
 
:<sup>4</sup>He + <sup>4</sup>He + 92 keV → [[Isotopes of beryllium|<sup>8*</sup>Be]]
:<sup>4</sup>He + <sup>8*</sup>Be + 67 keV → <sup>12*</sup>C
:<sup>12*</sup>C → [[Carbon-12|<sup>12</sup>C]] + γ + 7.4 MeV
 
For an overall reaction of:
 
:3<sup>4</sup>He → <sup>12</sup>C + γ + 7.2 MeV
 
In massive stars, heavier elements can also be burned in a contracting core through the [[neon burning process]] and [[oxygen burning process]]. The final stage in the stellar nucleosynthesis process is the [[silicon burning process]] that results in the production of the stable isotope iron-56. Fusion can not proceed any further except through an [[endothermic]] process, and so further energy can only be produced through gravitational collapse.<ref name="synthesis" />
 
The example below shows the amount of time required for a star of 20 solar masses to consume all of its nuclear fuel. As an O-class main sequence star, it would be 8 times the solar radius and 62,000 times the Sun's luminosity.<ref>{{cite journal | last1=Woosley | first1=S. E. | last2=Heger | first2=A. | last3=Weaver | first3=T. A. | title=The evolution and explosion of massive stars | journal=Reviews of Modern Physics | year=2002 | volume=74 | issue=4 | pages=1015–1071 | bibcode=2002RvMP...74.1015W | doi = 10.1103/RevModPhys.74.1015}}</ref>
{{-}}
{| class="wikitable" style="margin: 1em auto 1em auto;"
|-
!valign="bottom"| Fuel<br />material
!valign="bottom"| Temperature<br />(million kelvins)
!valign="bottom"| Density<br />(kg/cm<sup>3</sup>)
!valign="bottom"| Burn duration<br />(τ in years)
|- style="text-align:center;"
|| H
|| 37
|| 0.0045
|| 8.1 million
|- style="text-align:center;"
|| He
|| 188
|| 0.97
|| 1.2 million
|- style="text-align:center;"
|| C
|| 870
|| 170
|| 976
|- style="text-align:center;"
|| Ne
|| 1,570
|| 3,100
|| 0.6
|- style="text-align:center;"
|| O
|| 1,980
|| 5,550
|| 1.25
|- style="text-align:center;"
|| S/Si
|| 3,340
|| 33,400
|| 0.0315<ref>11.5 days is 0.0315 years.</ref>
|}
 
==See also==
{{Portal|Star|Astronomy}}
* [[Lists of stars]]
* [[List of largest stars]]
* [[List of astronomy topics#Stars and stellar objects|List of star-related topics]]
* [[Sidereal clock]]
* [[Star clock]]s
* [[Star count]]
* [[Stars and planetary systems in fiction]]
* [[Stellar astronomy]]
* [[Stellar dynamics]]
* ''[[Twinkle twinkle little star]]'' (nursery rhyme)
 
==References==
{{Reflist|colwidth=30em|refs=
<ref name=koch95>{{cite book | last1=Koch-Westenholz | first1=Ulla | last2=Koch | first2=Ulla Susanne | year=1995 | title=Mesopotamian astrology: an introduction to Babylonian and Assyrian celestial divination | page=163 | volume=19 | series=Carsten Niebuhr Institute Publications | publisher=Museum Tusculanum Press | isbn=87-7289-287-0 }}</ref>
<ref name=space_law09>{{cite book | last1=Lyall | first1=Francis | last2=Larsen | first2=Paul B. | title=Space Law: A Treatise | page=176 | publisher=Ashgate Publishing, Ltd | year=2009 | isbn=0-7546-4390-5 | chapter=Chapter 7: The Moon and Other Celestial Bodies }}</ref>
<ref name=astrometry05>{{cite web | title=Star naming | year=2005 | publisher=Scientia Astrophysical Organization. | url=http://www.astrometry.org/starnaming.php | accessdate=2010-06-29 }}</ref>
<ref name=bl_disclaimer>{{cite web | title=Disclaimer: Name a star, name a rose and other, similar enterprises | work=British Library | publisher=The British Library Board | url=http://www.bl.uk/names.html | archiveurl=http://web.archive.org/web/20100119033625/http://www.bl.uk/names.html | archivedate=2010-01-19 | accessdate=2010-06-29 }}</ref>
<ref name=andersen10>{{cite web | first=Johannes | last=Andersen | title=Buying Stars and Star Names | publisher=International Astronomical Union | url=http://www.iau.org/public/buying_star_names/ | accessdate=2010-06-24 }}</ref>
<ref name=si30_5>{{cite journal | first=Phil | last=Pliat | title=Name Dropping: Want to Be a Star? | journal=Skeptical Inquirer | volume=30.5 | date=September/October 2006 | url=http://www.csicop.org/si/show/name_dropping_want_to_be_a_star/ | accessdate=2010-06-29 }}</ref>
<ref name=sd19980401>{{cite web | last=Adams | first=Cecil | date=April 1, 1998 | title=Can you pay $35 to get a star named after you? | url=http://www.straightdope.com/columns/read/826/can-you-pay-35-to-get-a-star-named-after-you | publisher=The Straight Dope | accessdate=2006-08-13 }}</ref>
<ref name=golden_faflick82>{{cite news | last1=Golden | first1=Frederick | last2=Faflick | first2=Philip | date=January 11, 1982 | title=Science: Stellar Idea or Cosmic Scam? | work=Times Magazine | publisher=Time Inc. | url=http://www.time.com/time/magazine/article/0,9171,925195,00.html | accessdate=2010-06-24 }}</ref>
<ref name=di_justo20011226>{{cite news | first=Patrick | last=Di Justo | date=December 26, 2001 | title=Buy a Star, But It's Not Yours | work=Wired | publisher=Condé Nast Digital | url=http://www.wired.com/techbiz/media/news/2001/12/49345 | accessdate=2010-06-29 }}</ref>
<ref name=pliat02>{{cite book | first=Philip C. | last=Plait | year=2002 | title=Bad astronomy: misconceptions and misuses revealed, from astrology to the moon landing 'hoax' | pages=237–240 | publisher=John Wiley and Sons | isbn=0-471-40976-6 }}</ref>
<ref name=sclafani19980508>{{cite news | first=Tom | last=Sclafani | date=May 8, 1998 | title=Consumer Affairs Commissioner Polonetsky Warns Consumers: "Buying A Star Won't Make You One" | publisher=National Astronomy and Ionosphere Center, Aricebo Observatory | url=http://www.naic.edu/~gibson/starnames/isr_news.html | accessdate=2010-06-24 }}</ref>
}}
 
==Further reading==
* {{cite book | first1=Cliff | last1=Pickover | authorlink = Cliff Pickover | year=2001 |title=The Stars of Heaven | publisher=Oxford University Press | isbn=0-19-514874-6}}
* {{cite book | first1=John | last1=Gribbin | authorlink = John Gribbin | first2=Mary | last2=Gribbin | year=2001 | title=Stardust: Supernovae and Life—The Cosmic Connection | publisher=[[Yale University Press]] | isbn=0-300-09097-8}}
* {{cite book | first1=Stephen | last2=Hawking | title=A Brief History of Time | authorlink=Stephen Hawking | year=1988 | publisher=Bantam Books | isbn=0-553-17521-1}}
 
==External links==
{{Wiktionary}}
* {{cite web | last=Kaler | first=James | title=Portraits of Stars and their Constellations | publisher=University of Illinois | url=http://stars.astro.illinois.edu/sow/sow.html | accessdate=2010-08-20 }}
* {{cite web | title=Query star by identifier, coordinates or reference code | work=SIMBAD | publisher=Centre de Données astronomiques de Strasbourg | url=http://simbad.u-strasbg.fr/simbad/sim-fid | accessdate=2010-08-20 }}
* {{cite web | title=How To Decipher Classification Codes | publisher=Astronomical Society of South Australia | url=http://www.assa.org.au/sig/variables/classifications.asp | accessdate=2010-08-20 }}
* {{cite web | title=Live Star Chart | publisher=Dobsonian Telescope Community | url=http://www.mydob.co.uk/community_star.php | accessdate=2010-08-20 }} View the stars above your location
* {{cite web | display-authors=1 | last1=Prialnick | first1=Dina | last2=Wood | first2=Kenneth | last3=Bjorkman | first3=Jon | last4=Whitney | first4=Barbara | last5=Wolff | first5=Michael | last6=Gray | first6=David | last7=Mihalas | first7=Dimitri | title=Stars: Stellar Atmospheres, Structure, & Evolution | year=2001 | publisher=University of St. Andrews | url=http://www-star.st-and.ac.uk/~kw25/teaching/stars/stars.html | accessdate=2010-08-20 }}
 
{{Star}}
 
[[Category:Light sources]]
[[Category:Stars|*]]
[[Category:Stellar astronomy]]
 
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