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| {{for|the novel Sidereal Time|Christopher Meredith}}
| | == Replica Louis Vuitton Uk Bags Please email them and explain == |
| '''Sidereal time''' {{IPAc-en|s|aɪ|ˈ|d|ɪər|i|ə|l}} is a time-keeping system [[astronomers]] use to keep track of the direction to point their [[telescopes]] to view a given [[star]] in the [[night sky]]. Briefly, sidereal time is a "time scale that is based on the [[rotation of the Earth|Earth's rate of rotation]] measured relative to the [[fixed stars]]."<ref>[[National Institute of Standards and Technology]] [NIST], Time and Frequency Division. "Time and Frequency from A to Z." http://www.nist.gov/pml/div688/grp40/enc-s.cfm</ref>
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| From a given [[observation point]], a star found at one location in the sky will be found at nearly the same location on another night at the same sidereal time. This is similar to how the time kept by a [[sundial]] can be used to find the location of the [[Sun]]. Just as the Sun and [[Moon]] appear to rise in the east and set in the west due to the rotation of the Earth, so do the stars. Both [[solar time]] and sidereal time make use of the regularity of the Earth's rotation about its polar axis, solar time following the Sun while sidereal time roughly follows the stars. More exactly, sidereal time is the angle, measured from the observer's meridian, along the celestial equator, to the [[great circle]] that passes through the March equinox and both poles, and is usually expressed in hours, minutes, and seconds.<ref>Urban, S. E. & Seidelmann, P. K. (ed.) (2013). ''Explanatory Supplement to the Astronomical Almanac''. Mill Valley, CA: University Science Books. Glossary, s.v. hour angle, hour circle, sidereal time.</ref> Common time on a typical clock measures a slightly longer cycle, accounting not only for the Earth's axial rotation but also for the Earth's annual revolution around the Sun of slightly less than 1 degree per day (in fact to the nearest arc-second, it takes 365.2422 days
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| to revolve therefore 360 degrees/365.2422 days = 0.9856 degrees or 59 arc-minutes, 8 arc-seconds per day, i.e., slightly
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| A [[mean]] '''sidereal day''' is about 23 hours, 56 minutes, 4.0916 seconds (23.9344699 hours or 0.99726958 mean solar days), the time it takes the Earth to make one rotation relative to the [[vernal equinox]].{{Clarify|date=March 2013}} (Due to [[nutation]], an actual sidereal day is not quite so constant.) The vernal equinox itself [[Precession of the equinoxes|precesses]] slowly westward relative to the fixed stars, completing one revolution in about 26,000 years, so the misnamed sidereal day ("sidereal" is derived from the Latin ''sidus'' meaning "star") is some 0.0084 seconds shorter than the Earth's period of rotation relative to the fixed stars.
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| Maps of the stars in the night sky use [[declination]] and [[right ascension]] as coordinates. These correspond to [[latitude]] and [[longitude]] respectively. While declination is measured in degrees, right ascension is measured in units of time, because it was most natural to name locations in the sky in connection with the time when they crossed the [[meridian (astronomy)|meridian]].
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| In the sky, the [[meridian (astronomy)|meridian]] is the imaginary north to south line that goes through the point directly overhead (the [[zenith]]). The right ascension of any object crossing the meridian is equal to the current local (apparent) sidereal time, ignoring for present purposes that part of the circumpolar region north of the north celestial pole (for an observer in the northern hemisphere) or south of the south celestial pole (for an observer in the southern hemisphere) that is crossing the meridian the other way.
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| Because the Earth orbits the Sun once a year, the sidereal time at any given place and time will gain about four minutes against local [[civil time]], every 24 hours, until, after a year has passed, one additional sidereal "day" has elapsed compared to the number of solar days that have gone by.
| | <li>[http://verdamilio.net/tonio/spip.php?article1279/ http://verdamilio.net/tonio/spip.php?article1279/]</li> |
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| ==Sidereal time and solar time==
| | <li>[http://www.fxjxb.com/news/html/?48464.html http://www.fxjxb.com/news/html/?48464.html]</li> |
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| [[Image:Sidereal Time en.PNG|framed|Sidereal time vs solar time. '''Above left''': a distant star (the small red circle) and the Sun are at [[culmination]], on the local meridian. ''Centre'': only the distant star is at culmination (a mean [[sidereal day]]). ''Right'': a few minutes later the Sun is on the local meridian again. A [[solar day]] is complete.]] | | <li>[http://www.592bbs.net/forum.php?mod=viewthread&tid=248210&fromuid=6333 http://www.592bbs.net/forum.php?mod=viewthread&tid=248210&fromuid=6333]</li> |
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| [[Solar time]] is measured by the apparent [[diurnal motion]] of the sun, and local noon in apparent solar time is the moment when the sun is exactly due south or north (depending on the observer's latitude and the season). A mean solar day (what we normally measure as a "day") is the average time between local solar noons ("average" since this varies slightly over the year).
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| The Earth makes one rotation around its axis in a sidereal day; during that time it moves a short distance (about 1°) along its orbit around the sun. So after a sidereal day has passed the Earth still needs to rotate slightly more before the sun reaches local noon according to solar time. A mean solar day is, therefore, nearly 4 minutes longer than a sidereal day.
| | </ul> |
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| The stars are so far away that the Earth's movement along its orbit makes nearly no difference to their apparent direction (see, however, [[parallax]]), and so they return to their highest point in a sidereal day.
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| Another way to see this difference is to notice that, relative to the stars, the Sun appears to move around the Earth once per year. Therefore, there is one fewer [[solar day]] per year than there are sidereal days. This makes a sidereal day approximately {{Fraction|365.24|366.24}} times the length of the 24-hour solar day, giving approximately 23 hours, 56 minutes, 4.1 seconds (86,164.1 seconds).
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| ==Precession effects==
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| The Earth's rotation is not a simple rotation around an axis that would always remain parallel to itself. The Earth's rotational axis itself rotates about a second axis, orthogonal to the Earth's orbit, taking about 25,800 years to perform a complete rotation. This phenomenon is called the [[Axial precession|precession of the equinoxes]]. Because of this precession, the stars appear to move around the Earth in a manner more complicated than a simple constant rotation.
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| For this reason, to simplify the description of Earth's orientation in astronomy and [[geodesy]], it is conventional to chart the positions of the stars in the sky according to [[right ascension]] and [[declination]], which are based on a frame that follows the Earth's precession, and to keep track of Earth's rotation, through sidereal time, relative to this frame as well. In this reference frame, Earth's rotation is close to constant, but the stars appear to rotate slowly with a period of about 25,800 years. It is also in this reference frame that the [[tropical year]], the year related to the Earth's seasons, represents one orbit of the Earth around the sun. The precise definition of a sidereal day is the time taken for one rotation of the Earth in this precessing reference frame. | |
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| ==Definition==
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| Sidereal time, at any moment (and at a given locality defined by its geographical longitude), more precisely Local Apparent Sidereal Time (LAST), is defined as the [[hour angle]] of the vernal equinox at that locality: it has the same value as the [[right ascension]] of any celestial body that is crossing the local [[meridian (astronomy)|meridian]] at that same moment.
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| At the moment when the vernal [[Equinox#Celestial coordinate systems|equinox]] crosses the local [[meridian (astronomy)|meridian]], Local Apparent Sidereal Time is 00:00. Greenwich Apparent Sidereal Time (GAST) is the hour angle of the vernal equinox at the [[prime meridian]] at Greenwich, England.
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| Local Sidereal Time at any locality differs from the Greenwich Sidereal Time value of the same moment, by an amount that is proportional to the [[longitude]] of the locality. When one moves eastward 15° in longitude, sidereal time is larger by one sidereal hour (note that it wraps around at 24 hours). Unlike the reckoning of local solar time in "time zones," incrementing by (usually) one hour, differences in local sidereal time are reckoned based on actual measured longitude, to the accuracy of the measurement of the longitude, not just in whole hours.
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| Apparent Sidereal Time (Local or at Greenwich) differs from Mean Sidereal Time (for the same locality and moment) by the Equation of the Equinoxes: This is a small difference in Right Ascension R.A. (<math>dRA</math>) (parallel to the equator), not exceeding about +/-1.2 seconds of time, due to [[nutation]], the complex 'nodding' motion of the Earth's polar axis of rotation. It corresponds to the current amount of the nutation in ([[ecliptic]]) longitude (<math>d\psi</math>) and to the current obliquity (<math>\epsilon</math>) of the [[ecliptic]], so that <math>dRA = d\psi*cos(\epsilon)</math> .
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| Greenwich Mean Sidereal Time (GMST) and [[UT1]] differ from each other in rate, with the second of sidereal time a little shorter than that of UT1, so that (as at 2000 January 1 noon) 1.002 737 909 350 795 second of mean sidereal time was equal to 1 second of Universal Time (UT1). The ratio varies slightly with time, reaching 1.002 737 909 409 795 after a century.<ref>P K Seidelmann (ed.) (1992), ''Explanatory Supplement to the Astronomical Almanac'', [http://books.google.com/books?id=uJ4JhGJANb4C&pg=PA52 at page 52] (and at page 698).</ref>
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| To an accuracy within 0.1 second per century, Greenwich (Mean) Sidereal Time (in hours and decimal parts of an hour) can be calculated as
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| :GMST = 18.697 374 558 + 24.065 709 824 419 08 * D ,
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| where D is the interval, in UT1 days including any fraction of a day, since 2000 January 1, at 12h UT (interval counted positive if forwards to a later time than the 2000 reference instant), and the result is freed from any integer multiples of 24 hours to reduce it to a value in the range 0–24.<ref>[http://aa.usno.navy.mil/faq/docs/GAST.php Approximate sidereal time (US Naval Observatory)].</ref>
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| In other words, Greenwich Mean Sidereal Time exceeds mean solar time at Greenwich by a difference equal to the longitude of the fictitious mean Sun used for defining mean solar time (with longitude converted to time as usual at the rate of 1 hour for 15 degrees), plus or minus an offset of 12 hours (because mean solar time is reckoned from 0h midnight, instead of the pre-1925 astronomical tradition where 0h meant noon).
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| Sidereal time is used at astronomical observatories because sidereal time makes it very easy to work out which astronomical objects will be observable at a given time. Objects are located in the night sky using [[right ascension]] and [[declination]] relative to the celestial equator (analogous to longitude and [[latitude]] on Earth), and when sidereal time is equal to an object's right ascension the object will be at its highest point in the sky, or ''culmination'', at which time it is usually best placed for observation, as atmospheric [[extinction (astronomy)|extinction]] is minimised.
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| Sidereal time is a measure of the position of the [[Earth]] in its rotation around its axis, or time measured by the apparent [[diurnal motion]] of the [[vernal equinox]], which is very close to, but not identical to, the motion of stars. They differ by the [[Precession (astronomy)|precession]] of the vernal equinox in [[right ascension]] relative to the stars.<br />Earth's '''sidereal day''' also differs from its [[rotation period]] relative to the background stars by the amount of precession in right ascension during one day (8.4 ms).<ref>Seidelmann, p. 48.</ref> Its [[J2000]] mean value is 23<sup>h</sup>56<sup>m</sup>4.090 530 833<sup>s</sup>.<ref name=Aoki>Aoki, S., B. Guinot, G. H. Kaplan, H. Kinoshita, D. D. McCarthy and P. K. Seidelmann: "[http://adsabs.harvard.edu/abs/1982A&A...105..359A The new definition of Universal Time]". ''Astronomy and Astrophysics'' '''105'''(2), 359–361, 1982.</ref>
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| ==Exact duration and its variation==
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| A mean sidereal day is about 23 h 56 m 4.1 s in length. However, due to variations in the rotation rate of the Earth, the rate of an ideal sidereal clock deviates from any simple multiple of a civil clock. In practice, the difference is kept track of by the difference [[UTC]]–[[UT1]], which is measured by radio telescopes and kept on file and available to the public at the [[IERS]] and at the [[United States Naval Observatory]].
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| Given a tropical year of 365.242 190 402 days from Simon et al.<ref>Simon, J. L., P. Bretagnon, J. Chapront, M. Chapront-Touzé, G Francou and J. Laskar: "[http://adsabs.harvard.edu/abs/1994A%26A...282..663S Numerical expressions for precession formulas and mean elements for the moon and the planets]". ''Astronomy and Astrophysics'' '''282''', 663–683, 1994.</ref> this gives a sidereal day of 86 400 × <math> \tfrac{365.242\ 190\ 402}{366.242\ 190\ 402} </math>, or 86 164.090 53 seconds.
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| Aoki et al.,<ref>Aoki, S., B. Guinot, G. H. Kaplan, H. Kinoshita, D. D. McCarthy and P. K. Seidelmann: "[http://adsabs.harvard.edu/abs/1982A&A...105..359A The new definition of Universal Time]". ''Astronomy and Astrophysics'' '''105'''(2), 361, 1982, see equation 19.</ref> defined UT1 such that the observed sidereal day at the beginning of 2000 would be {{Fraction|1|1.002 737 909 350 795}} times a UT1 day of 86 400 seconds, which gives 86 164.090 530 833 seconds of UT1. For times within a century of 1984, the ratio only alters in its 11th decimal place. This [http://tycho.usno.navy.mil/sidereal.html web-based sidereal time calculator] uses a truncated ratio of {{Fraction|1|1.002 737 909 35}}.
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| Because this is the period of rotation in a precessing reference frame, it is not directly related to the mean rotation rate of the Earth in an inertial frame, which is given by ω=2π/T where T is the slightly longer stellar day given by Aoki et al. as 86 164.098 903 697 32 seconds.<ref name=Aoki/> This can be calculated by noting that ω is the magnitude of the vector sum of the rotations leading to the sidereal day and the precession of that rotation vector. In fact, the period of the Earth's rotation varies on hourly to interannual timescales by around a [[millisecond]],<ref>Hide, R., and J. O. Dickey: "Earth's variable rotation". ''Science'' '''253''' (1991) 629–637.</ref> together with a secular increase in length of day of about 2.3 milliseconds per century, mostly from [[tidal acceleration|tidal friction]] slowing the Earth's rotation.<ref>Stephenson, F.R. ''Historical eclipses and Earth's rotation''. Cambridge University Press, 1997, 557pp.</ref>
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| ==Sidereal days compared to solar days on other planets==
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| Of the eight solar [[planet]]s,<ref>Bakich, Michael E., ''The Cambridge Planetary Handbook'', Cambridge University Press, 2000; ISBN 0-521-63280-3.</ref> all but [[Venus]] and [[Uranus]] have [[prograde motion|prograde]] rotation—that is, they rotate more than once per year in the same direction as they orbit the sun, so the sun rises in the east. Venus and Uranus, however, have [[retrograde motion|retrograde]] rotation. For prograde rotation, the formula relating the lengths of the sidereal and solar days is
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| :<math> \text{number of sidereal days per orbital period}=1+ \text{number of solar days per orbital period}</math> | |
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| or equivalently
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| :<math> \text{length of solar day}=\frac{\text{length of sidereal day}}{1- \tfrac{\text{length of sidereal day}}{\text{orbital period}}}. </math>
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| On the other hand, the formula in the case of retrograde rotation is
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| :<math>\text{number of sidereal days per orbital period}= -1+ \text{number of solar days per orbital period}</math>
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| or equivalently
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| :<math>\text{length of solar day}=\frac{\text{length of sidereal day}}{1+ \tfrac{\text{length of sidereal day}}{\text{orbital period}}}. </math>
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| All the solar planets more distant from the sun than Earth are similar to Earth in that, since they experience many rotations per revolution around the sun, there is only a small difference between the length of the sidereal day and that of the solar day—the ratio of the former to the latter never being less than Earth's ratio of .997 . But the situation is quite different for [[Mercury (planet)|Mercury]] and Venus. Mercury's sidereal day is about two-thirds of its orbital period, so by the prograde formula its solar day lasts for two revolutions around the sun—three times as long as its sidereal day. Venus rotates retrograde with a sidereal day lasting about 243.0 earth-days, or about 1.08 times its orbital period of 224.7 earth-days; hence by the retrograde formula its solar day is about 116.8 earth-days, and it has about 1.9 solar days per orbital period.
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| By convention, rotation periods of planets are given in sidereal terms unless otherwise specified.
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| ==See also== | |
| * [[Earth rotation]]
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| * [[Sidereal month]]
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| * [[Synodic day]]
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| * [[Anti-sidereal time]]
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| * [[Nocturnal (instrument)]]
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| * [[Transit instrument]]
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| ==References==
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| {{reflist}}
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| *P. Kenneth Seidelmann, ed., ''Explanatory supplement to the Astronomical Almanac'', (Mill Valley, Cal.: University Science Books, 1992)
| |
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| ==External links==
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| {{wiktionary|sidereal time}}
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| * [http://tycho.usno.navy.mil/sidereal.html Web based Sidereal time calculator]
| |
| * [https://itunes.apple.com/us/app/celestial-clock/id626626736 App version for iOS devices]
| |
| * [http://www.longavista.com.br/sideral.htm Build an internet synchronized sidereal clock]
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| * For more details, see the [http://docs.kde.org/en/3.1/kdeedu/kstars/ai-sidereal.html article on sidereal time] from Jason Harris' Astroinfo.
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| {{Time Topics}}
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| {{Time measurement and standards}}
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| {{DEFAULTSORT:Sidereal Time}}
| |
| [[Category:Units of time]]
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| [[Category:Horology]]
| |
| [[Category:Time scales]]
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| [[Category:Time in astronomy]]
| |
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WHAT TO WEAR: A week out and climate is predicted to be in the 40's at night, but once the sun comes up so will the temperature. As all good Coloradans, think layers. We will be walking but there will be moments of stopping to photograph too. I also recommend bringing some water. For people with that are hair challenged, I recommend a hat as there isn't many trees to safeguard from the sun and the morning might be chilly before the sun rises.
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Untrained observers could detect narcissism, too. They found that the observers used three characteristics volume of social interaction, attractiveness of the individual and the degree of self promotion in the main photo to form an impression of the individual's personality. "People aren't perfect within their assessments," Buffardi said, "but our results show they're somewhat accurate in their judgments."
If you are one of those Folks who sends me invitations to Fieldville, Zillionare City or Gang Wars, quit it, nobody likes that shit, but when you are one of those Folks who likes to browse Facebook from the commodity of your toiletyour cellphone,you may want to know this: Facebook app manufacturers may be spying on you!! That right, and not only your likes and preferences but additionally your phone calls, text messages as well as tracking your location!! If you are using Facebook via your Smartphone or iPhone, chances are that you might be spied on!
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