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| {{Planetbox begin
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| | name = [[Harvard Revised catalogue|HR]] 8799 b
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| }}
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| {{Planetbox image
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| | image = Exoplanet Comparison HR 8799 b.png
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| | caption = Size comparison of HR 8799 b (gray) with Jupiter.
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| }}
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| {{Planetbox star
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| | star = [[HR 8799]]
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| | constell = [[Pegasus (constellation)|Pegasus]]
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| | RA = {{RA|23|07|28.7150}}<ref name="SIMBAD">{{SIMBAD link|HR+8799|V* V342 Peg -- Variable Star of gamma Dor type}}, entry, [[SIMBAD]]. Accessed on line November 14, 2008.</ref>
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| | DEC = {{DEC|+21|08|03.302}}<ref name="SIMBAD" />
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| | app_mag = 5.964<ref name="SIMBAD" />
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| | dist_ly = 129 ± 4<ref name="vanLeeuwen2007">{{cite web|url=http://webviz.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=I/311/hip2&recno=113804|title=HIP 114189|work=Hipparcos, the New Reduction|author=van Leeuwen, F.|year=2007|accessdate=2008-10-13}}</ref><ref group="note" name="calculate_distance">Computed from parallax: <math>\scriptstyle \mathrm{distance\ in\ parsecs}=\frac{1000}{\mathrm{parallax\ in\ milliarcseconds}}</math></ref>
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| | dist_pc = 39 ± 1<ref name="vanLeeuwen2007" /><ref group="note" name="calculate_distance" />
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| | class = kA5 hF0 mA5 V; λ Boo<ref name="Gray1999">{{cite journal|title=HR 8799: A Link between γ Doradus Variables and λ Bootis Stars|author=Gray, R.O. and Kaye, A.B.|year=1999|journal=[[The Astronomical Journal]]|volume=118|issue=6|pages=2993–2996|doi=10.1086/301134|bibcode=1999AJ....118.2993G}}</ref><ref name="Kaye1999">{{cite journal|title=Gamma Doradus Stars: Defining a New Class of Pulsating Variables|author=Kaye, A.B. ''et al.''|year=1999|journal=[[PASP]]|volume=111|issue=761|pages=840–844|bibcode=1999PASP..111..840K|doi=10.1086/316399|arxiv = astro-ph/9905042 }}</ref>
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| }}
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| {{Planetbox separation
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| | epoch = 2008-09-18
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| | separation_mas = 1724<ref name="Marois2008">{{cite journal |last=Marois |first=Christian |authorlink= |coauthors=''et al.'' |date=November 2008 |title=Direct Imaging of Multiple Planets Orbiting the Star HR 8799 |journal=[[Science (journal)|Science]] |volume=322 |issue=5906 |pages=1348–1352 |doi=10.1126/science.1166585 |arxiv=0811.2606 |accessdate= |quote= |pmid=19008415 |bibcode = 2008Sci...322.1348M }}</ref><ref group="note" name="separation">Calculated from the separations in the East and North directions which are 1.528 and 0.798 [[arcsecond]]s respectively.</ref>
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| | position_angle = 62.42<ref name="Marois2008" /><ref group="note" name="separation" />
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| | separation = 68<ref name="Marois2008" />
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| }}
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| {{Planetbox orbit
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| | semimajor = ~ 68<ref name="Marois2008" /><ref group="note" name="circular_orbit">Value given assuming the planet's orbit is circular and is being observed face-on.</ref>
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| | semimajor_gm = ~ 10000
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| | period_year = ~ 460<ref name="Marois2008" /><ref group="note" name="circular_orbit" />
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| }}
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| {{Planetbox character
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| | mass = 5{{±|2|1}}<ref name="cite arxiv |eprint=1011.4918">{{cite arxiv |eprint=1011.4918 |author1=Marois |author2=Zuckerman |author3=Konopacky |author4=Macintosh |author5=Barman |title=Images of a fourth planet orbiting HR 8799 |class=astro-ph.EP |year=2010}}</ref>
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| | radius = 1.2 ± 0.1<ref name="Marois2008" />
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| | density = 2.91{{±|1|0.7}}
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| | temperature = 870{{±|30|70}}<ref name="Marois2008" />
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| }}
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| {{Planetbox discovery
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| | discovery_date = November 13, 2008
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| | discoverers = Marois ''et al.''
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| | discovery_method = [[Direct imaging]]
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| | discovery_site = [[W.M. Keck Observatory|Keck]] and [[Gemini Observatory|Gemini<br/>observatories]] in [[Hawaii]]
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| | discovery_status = Published
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| }}
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| {{Planetbox catalog
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| | names = [[Henry Draper catalogue|HD]] 218396 b<ref>{{SIMBAD link|HD+218396b|HD 218396b -- Extra-solar Planet Candidate}}, entry, [[SIMBAD]]. Accessed on line December 6, 2008.</ref>
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| }}
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| {{Planetbox reference
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| | star = HR+8799
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| | planet = b
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| | simbad = HD+218396b
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| }}
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| {{Planetbox end}}
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| '''HR 8799 b''' is an [[extrasolar planet]] located approximately 129 [[light-year]]s away in the [[constellation]] of [[Pegasus (constellation)|Pegasus]], orbiting the 6th [[apparent magnitude|magnitude]] [[Lambda Boötis star]] [[HR 8799]]. It has a mass between 4 and 7 <ref name="cite arxiv |eprint=1011.4918"/>[[Jupiter mass]]es and a radius from 10 to 30% larger than [[Jupiter]]'s. It orbits at 68 [[astronomical units|AU]] from HR 8799 (or 7 AU inside the inner edge of the [[dust disk]] orbiting the star) with an unknown eccentricity and a period of 460 years, and is the outermost known planet in the HR 8799 system. Along with two other planets orbiting HR 8799, the planet was discovered on November 13, 2008 by Marois ''et al.'', using the [[W.M. Keck Observatory|Keck]] and [[Gemini Observatory|Gemini observatories]] in [[Hawaii]]. These planets were discovered using the [[direct imaging]] technique.<ref name="Marois2008" /><ref>{{cite press release|url=http://www.keckobservatory.org/article.php?id=231|title=Astronomers capture first images of newly-discovered solar system|publisher=W. M. Keck Observatory|date=2008-11-13|accessdate=2008-12-02}}</ref><ref>{{cite press release|url=http://www.gemini.edu/node/11151|title=Gemini Releases Historic Discovery Image of Planetary First Family|publisher=Gemini Observatory|date=2008-11-13|accessdate=2008-12-02}}</ref><ref>{{cite news|title=Scientists Publish First Direct Images of Extrasolar Planets|first=Joel|last=Achenbach|work=[[The Washington Post]]|publisher=[[The Washington Post Company]]|date=2008-11-13|accessdate=2008-12-02|url=http://www.washingtonpost.com/wp-dyn/content/article/2008/11/13/AR2008111302267.html}}</ref><ref>{{cite journal |title=Stability of the directly imaged multiplanet system HR 8799: resonance and masses |author=Fabrycky ''et al.'' |date=1 December 2008|pages=1408–1421 |accessdate=2008-12-02 |issue=2 |volume=710 |author2=Murray-Clay |doi=10.1088/0004-637X/710/2/1408 |journal=Astrophys.J. |arxiv=0812.0011|bibcode = 2010ApJ...710.1408F }}</ref>
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| [[Image:Planet around HR 8799.jpg|thumb|left|An artist's impression of HR 8799 b viewed from a moon.]]
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| In 2009 it was discovered that the [[Hubble Space Telescope]] had in fact directly imaged HR 8799 b eleven years earlier, in 1998, suggesting that more exoplanets might be revealed through analysis of HST photographic archives.<ref>{{cite journal |title=HST/NICMOS detection of HR 8799 b in 1998 |author= Lafrenière ''et al.'' |date=18 February 2009|accessdate=2009-04-01 |doi=10.1088/0004-637X/694/2/L148 |last2=Marois |first2=Christian |last3=Doyon |first3=René |last4=Barman |first4=Travis |journal=The Astrophysical Journal |volume=694 |issue=2 |pages=L148–L152 |arxiv=0902.3247}}</ref> Additional precovery images were also obtained by reanalyzing data taken in 2002 at the Subaru Telescope and in 2005 and 2007 at the W.M Keck Observatory
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| <ref name="Fukagawa2009">{{cite journal |last=Fukagawa |first=Misato |authorlink= |coauthors=''et al.'' |date=July 2012 |title=H-Band Image of a Planetary Companion Around HR 8799 in 2002 |journal=[[The Astrophysical Journal Letters|ApJL]] |volume=696|pages=1 |arxiv=1206.0483 |bibcode = 2009ApJ...696L...1F}}</ref>
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| <ref name="Metchev2009">{{cite journal |last=Metchev |first=Stanimir |authorlink= |coauthors=''et al.'' |date=November 2009 |title=Pre-Discovery 2007 Image of the HR 8799 Planetary System |journal=[[The Astrophysical Journal Letters|ApJL]] |volume=696|pages=1 |arxiv=0910.0915|bibcode = 2009ApJ...705L.204M}}</ref>
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| .<ref name="Currie2012">{{cite journal |last=Currie |first=Thayne |authorlink= |coauthors=''et al.'' |date=July 2012 |title=Direct Detection and Orbital Analysis of the Exoplanets HR 8799 bcd from Archival 2005 Keck/NIRC2 Data |journal=[[The Astrophysical Journal Letters|ApJL]] |volume=755 |pages=34 |arxiv=1206.0483 |bibcode = 2012ApJ...755L..34C}}</ref>
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| Broadband photometry of HR 8799 b shows that it has thicker clouds in its atmosphere than do older, higher surface gravity substellar objects of the same effective temperature.<ref name="Currie2011">{{cite journal |last=Currie |first=Thayne |authorlink= |coauthors=''et al.'' |date=March 2011 |title=A Combined Subaru/VLT/MMT 1--5 Micron Study of Planets Orbiting HR 8799: Implications for Atmospheric Properties, Masses, and Formation |journal=[[The Astrophysical Journal|ApJ]] |volume=729 |issue=2|pages=128 |arxiv=1101.1973 |bibcode = 2011ApJ...729..128C }}</ref>
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| Near infrared H band and K band spectroscopy of HR8799b published in May 2011 indicate a hydrogen rich, dusty atmosphere with disequilibrium CO / CH4 chemistry.<ref>{{cite paper|url=http://arxiv.org/pdf/1103.3895v1|title=Clouds and Chemistry in the Atmosphere of Extrasolar Planet HR8799b|publisher=Cornell University Library|date=2011-03-20|accessdate=2011-03-20}}</ref>
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| Near infrared spectroscopy from 995 to 1769 nanometers made with the Palomar Obervatory show evidence of Ammonia and/or Acetylene as well as Carbon Dioxide, but little Methane.<ref name=Gilliland>{{cite web|first = B. R. Oppenheimer|title= Reconnaissance of the HR 8799 Exosolar System I: Near IR Spectroscopy|url=http://arxiv.org/abs/1303.2627|publisher=Cornell University|accessdate=12 March 2013}}</ref>
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| __NOTOC__
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| ==Notes==
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| <references group="note" /> | |
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| ==See also==
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| * [[Fomalhaut b]]
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| | |
| ==References==
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| {{reflist}}
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| | |
| ==External links==
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| {{Commons category-inline}}
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| * {{cite web | url=http://media4.obspm.fr/exoplanets/base/planete.php?etoile=HR+8799&planete=b | title=HR 8799 b | work=Exoplanets}}
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| {{HR 8799}}
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| {{Sky|23|07|28.7150|+|21|08|03.302|129}}
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| | |
| {{DEFAULTSORT:Hr 8799 B}}
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| [[Category:HR 8799]]
| |
| [[Category:Exoplanets discovered in 2008]]
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| [[Category:Gas giants]]
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| [[Category:Pegasus (constellation)]]
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| [[Category:Exoplanets detected by direct imaging]]
| |
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