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| epoch = J2000 |
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| epoch = J2000 |
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| constell = ] |
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| constell = ] |
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| ra = {{RA|23|13|16.97632}}<ref name=aaa474_2_653/> |
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| ra = {{RA|23|13|16.97496}}<ref name="GaiaDR3"/> |
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| dec = {{DEC|+57|10|06.0823}}<ref name=aaa474_2_653/> |
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| dec = {{DEC|+57|10|06.0838}}<ref name="GaiaDR3"/> |
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| appmag_v = 5.574<ref name=aaass65_2_405/> |
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| appmag_v = 5.574<ref name=aaass65_2_405/> |
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{{Starbox astrometry |
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{{Starbox astrometry |
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| radial_v = –18.5<ref name=scfs/> |
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| radial_v = {{val|-18.68|0.12}}<ref name="GaiaDR3"/> |
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| prop_mo_ra = +{{val|2075.07|0.33}}<ref name=aaa474_2_653/> |
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| prop_mo_ra = {{val|2074.414|0.050}} |
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| prop_mo_dec = +{{val|295.45|0.25}}<ref name=aaa474_2_653/> |
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| prop_mo_dec = {{val|294.452|0.043}} |
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| pm_footnote = <ref name="GaiaDR3"/> |
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| parallax = 152.8640 |
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| parallax = 152.8640 |
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| p_error = 0.0494 |
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| p_error = 0.0494 |
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| parallax_footnote = <ref name="GaiaEDR3">{{Cite Gaia EDR3|2009481748875806976}}</ref> |
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| parallax_footnote = <ref name="GaiaDR3"/> |
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| absmag_v = 6.46<ref name=Holmberg2009/> |
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| absmag_v = 6.46<ref name=Holmberg2009/> |
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'''HD 219134''' (also known as '''Gliese 892''' or '''HR 8832''') is a ] star in the ] of ]. It is smaller and less luminous than the ], with a ] of K3V, which makes it an orange-hued star. HD 219134 is relatively close to our system, with an estimated distance of 21.25 ]s. This star is close to the limit of ] that can still be seen by the unaided eye. The limit is considered to be magnitude 6 for most observers. This star has a magnitude 9.4 optical companion at an angular separation of 106.6 ]s.<ref name=mnras389_2_869/> |
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'''HD 219134''' (also known as '''Gliese 892''' or '''HR 8832''') is a ] star in the ] of ]. It is smaller and less luminous than the ], with a ] of K3V, which makes it an orange-hued star. HD 219134 is relatively close to our system, with an estimated distance of 21.34 ]s. This star is close to the limit of ] that can still be seen by the unaided eye. The limit is considered to be magnitude 6 for most observers. This star has a magnitude 9.4 optical companion at an angular separation of 106.6 ]s.<ref name=mnras389_2_869/> |
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== Planetary system == |
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== Planetary system == |
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HD 219134 has a system of 6 ]s. The innermost planet, ], is a rocky ] based on size (1.6 times the size of Earth), and density (6.4 grams per cubic cm).<ref name="NASA-20150730">{{cite web |title=PIA19832: Location of Nearest Rocky Exoplanet Known |url=http://photojournal.jpl.nasa.gov/catalog/PIA19832 |date=30 July 2015 |work=] |access-date=30 July 2015 }}</ref><ref name="NASA-20150730-fc">{{cite web |last1=Chou |first1=Felicia |last2=Clavin |first2=Whitney |title=NASA's Spitzer Confirms Closest Rocky Exoplanet |url=http://www.jpl.nasa.gov/news/news.php?feature=4672 |date=30 July 2015 |work=] |access-date=31 July 2015 }}</ref> This and three additional exoplanets; one ] (designated ''c'' and later found to be rocky as well), one ] world (''d''), and one ] world (''e''); were deduced using HARPS-N radial velocity data by Motalebi ''et al.'' in 2015.<ref name="Motalebi2015" /><ref name="Harvard-Smithsonian-Release No.2015-1">{{cite web |title= Cassiopeia's Hidden Gem |url=https://www.cfa.harvard.edu/news/2015-16|date=30 July 2015 |work=] |access-date=30 July 2015 }}</ref> Two months later, Vogt ''et al.'' published a paper on this system which found a 6-planet solution, with planets ''b'' & ''c'' corresponding to those in Motalebi ''et al.'', ''e'' & ''g'' corresponding to Motalebi's ''d'' & ''e'', and ''d'' & ''f'' being new planets.<ref name="Vogt2015" /><ref group="note">The ] redesignated Vogt's ''d'' & ''f'' as ''f'' & ''g'' for consistency with Motalebi ''et al.'', and initially incorrectly listed Vogt's ''g'' as a separate planet from Motalebi's ''e'' due to the difference in reported parameters, introducing the designation ''h'' for it. The Exoplanet Archive designations have been used in subsequent papers on this system. (See also the Johnson ''et al.'' 2016 reference.)</ref><ref name="Johnson2016" /> A total of four independent studies have been done regarding the planetary system of HD 219134, with some of their results conflicting with each other. As of March 2017, the star is known to have at least 5 planets, with two of them (HD 219134 b and c) known to be transiting, rocky super-Earths. The previously reported planets HD 219134 g and h were not reported in following HARPS-N analyses in March 2017 by Gillon ''et al''.<ref name="Gillon2017" /><ref>{{Cite web|url=http://backalleyastronomy.blogspot.com/2017/04/hd-219134-scorecard-5-planets-2.html?m=1|title=Back Alley Astronomy: HD 219134 Scorecard: 5 planets, 2 transiting|date=18 April 2017}}</ref><!-- The blog source suggests planet g is disputed, but the paper does not. --> |
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HD 219134 has a system of six known ]s. The innermost planet, ], is a rocky ] based on size (1.6 times the size of Earth), and density (6.4 grams per cubic cm).<ref name="NASA-20150730">{{cite web |title=PIA19832: Location of Nearest Rocky Exoplanet Known |url=http://photojournal.jpl.nasa.gov/catalog/PIA19832 |date=30 July 2015 |work=] |access-date=30 July 2015 }}</ref><ref name="NASA-20150730-fc">{{cite web |last1=Chou |first1=Felicia |last2=Clavin |first2=Whitney |title=NASA's Spitzer Confirms Closest Rocky Exoplanet |url=http://www.jpl.nasa.gov/news/news.php?feature=4672 |date=30 July 2015 |work=] |access-date=31 July 2015 }}</ref> This and three additional exoplanets; one ] (designated ''c'' and later found to be rocky as well), one ] world (''d''), and one ] world (''e''); were deduced using HARPS-N radial velocity data by Motalebi ''et al.'' in 2015.<ref name="Motalebi2015" /><ref name="Harvard-Smithsonian-Release No.2015-1">{{cite web |title= Cassiopeia's Hidden Gem |url=https://www.cfa.harvard.edu/news/2015-16|date=30 July 2015 |work=] |access-date=30 July 2015 }}</ref> Two months later, Vogt ''et al.'' published a paper on this system which found a 6-planet solution, with planets ''b'', ''c'' & ''d'' corresponding to those in Motalebi ''et al.'', ''f'' & ''g'' being new planets, and ''h'' corresponding to Motalebi's ''e'' but with different, and more accurate, estimated parameters.<ref name="Vogt2015" /><ref name="Johnson2016" /> |
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A number of independent studies have been done regarding the planetary system of HD 219134, with some of their results conflicting with each other. As of March 2017, the star is known to have at least 5 planets, with two of them (HD 219134 b and c) known to be transiting, rocky super-Earths. The previously reported planets HD 219134 g and h were not reported in following HARPS-N analyses in March 2017 by Gillon ''et al''.<ref name="Gillon2017" /><ref>{{Cite web|url=http://backalleyastronomy.blogspot.com/2017/04/hd-219134-scorecard-5-planets-2.html?m=1|title=Back Alley Astronomy: HD 219134 Scorecard: 5 planets, 2 transiting|date=18 April 2017}}</ref><!-- The blog source suggests planet g is disputed, but the paper does not. --> |
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{{OrbitboxPlanet begin |
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{{OrbitboxPlanet begin |
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==References== |
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==References== |
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{{Reflist|refs= |
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<ref name="GaiaDR3">{{Cite Gaia DR3|2009481748875806976}}</ref> |
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<ref name=Holmberg2009>{{citation |
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<ref name=Holmberg2009>{{citation |
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| arxiv=0811.3982 | s2cid=118577511 | postscript=. }}</ref> |
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| arxiv=0811.3982 | s2cid=118577511 | postscript=. }}</ref> |
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<ref name=aaa474_2_653>{{citation | first=F. | last=van Leeuwen |date=November 2007 | title=Validation of the new Hipparcos reduction | journal=Astronomy and Astrophysics | volume=474 | issue=2 | pages=653–664 | bibcode=2007A&A...474..653V | doi=10.1051/0004-6361:20078357 | postscript=. |arxiv = 0708.1752 | s2cid=18759600 }}</ref> |
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<ref name=aaa508_3_1313>{{citation | display-authors=1 | last1=Frasca | first1=A. | last2=Covino | first2=E. | last3=Spezzi | first3=L. | last4=Alcalá | first4=J. M. | last5=Marilli | first5=E. | last6=Fżrész | first6=G. | last7=Gandolfi | first7=D. | title=REM near-IR and optical photometric monitoring of pre-main sequence stars in Orion. Rotation periods and starspot parameters | journal=Astronomy and Astrophysics | volume=508 | issue=3 | pages=1313–1330 |date=December 2009 | doi=10.1051/0004-6361/200913327 | bibcode=2009A&A...508.1313F | postscript=. | arxiv=0911.0760 | s2cid=118361131 }}</ref> |
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<ref name=aaa508_3_1313>{{citation | display-authors=1 | last1=Frasca | first1=A. | last2=Covino | first2=E. | last3=Spezzi | first3=L. | last4=Alcalá | first4=J. M. | last5=Marilli | first5=E. | last6=Fżrész | first6=G. | last7=Gandolfi | first7=D. | title=REM near-IR and optical photometric monitoring of pre-main sequence stars in Orion. Rotation periods and starspot parameters | journal=Astronomy and Astrophysics | volume=508 | issue=3 | pages=1313–1330 |date=December 2009 | doi=10.1051/0004-6361/200913327 | bibcode=2009A&A...508.1313F | postscript=. | arxiv=0911.0760 | s2cid=118361131 }}</ref> |
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<ref name=scfs>{{citation | display-authors=1 | title=Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic fundamental stars with direct solutions | journal=Veröff. Astron. Rechen-Inst. Heidelb | volume=35 | last1=Wielen | first1=R. | last2=Schwan | first2=H. | last3=Dettbarn | first3=C. | last4=Lenhardt | first4=H. | last5=Jahreiß | first5=H. | last6=Jährling | first6=R. | publisher=Astronomisches Rechen-Institut Heidelberg | issue=35 | pages=1 | year=1999 | bibcode=1999VeARI..35....1W | postscript=. }}</ref> |
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<ref name=aaa520_A79>{{citation | display-authors=1 | last1=Martínez-Arnáiz | first1=R. | last2=Maldonado | first2=J. | last3=Montes | first3=D. | last4=Eiroa | first4=C. | last5=Montesinos | first5=B. | title=Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter | journal=Astronomy and Astrophysics | volume=520 | page=A79 |date=September 2010 | doi=10.1051/0004-6361/200913725 | bibcode=2010A&A...520A..79M | postscript=. |arxiv = 1002.4391 | s2cid=43455849 | url=http://eprints.ucm.es/37826/1/davidmontes17libre.pdf }}</ref> |
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<ref name=aaa520_A79>{{citation | display-authors=1 | last1=Martínez-Arnáiz | first1=R. | last2=Maldonado | first2=J. | last3=Montes | first3=D. | last4=Eiroa | first4=C. | last5=Montesinos | first5=B. | title=Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter | journal=Astronomy and Astrophysics | volume=520 | page=A79 |date=September 2010 | doi=10.1051/0004-6361/200913725 | bibcode=2010A&A...520A..79M | postscript=. |arxiv = 1002.4391 | s2cid=43455849 | url=http://eprints.ucm.es/37826/1/davidmontes17libre.pdf }}</ref> |
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<ref name=mnras389_2_869>{{citation | last1=Eggleton | first1=P. P. | last2=Tokovinin | first2=A. A. | title=A catalogue of multiplicity among bright stellar systems | journal=] | volume=389 | issue=2 | pages=869–879 |date=September 2008 | doi=10.1111/j.1365-2966.2008.13596.x | bibcode=2008MNRAS.389..869E | postscript=. |arxiv = 0806.2878 | s2cid=14878976 }}</ref> |
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<ref name=mnras389_2_869>{{citation | last1=Eggleton | first1=P. P. | last2=Tokovinin | first2=A. A. | title=A catalogue of multiplicity among bright stellar systems | journal=] | volume=389 | issue=2 | pages=869–879 |date=September 2008 | doi=10.1111/j.1365-2966.2008.13596.x | bibcode=2008MNRAS.389..869E | postscript=. |arxiv = 0806.2878 | s2cid=14878976 }}</ref> |
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<!-- <ref name=apjss168_2_297>{{citation | display-authors=1 | last1=Takeda | first1=Genya | last2=Ford | first2=Eric B. | last3=Sills | first3=Alison | last4=Rasio | first4=Frederic A. | last5=Fischer | first5=Debra A. | last6=Valenti | first6=Jeff A. | title=Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog | journal=The ] Supplement Series | volume=168 | issue=2 | pages=297–318 |date=February 2007 | doi=10.1086/509763 | bibcode=2007ApJS..168..297T | arxiv=astro-ph/0607235 | postscript=. }}</ref> --> |
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<ref name="Motalebi2015">{{cite journal |arxiv=1507.08532 |last1=Motalebi |first1=F. |display-authors=etal |title=The HARPS-N Rocky Planet Search. I. HD 219134 b: A transiting rocky planet in a multi-planet system at 6.5 pc from the Sun |date=December 2015 |doi=10.1051/0004-6361/201526822 |volume=584 |journal=] |page=A72 |bibcode=2015A&A...584A..72M |s2cid=45652878 }}</ref> |
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<ref name="Motalebi2015">{{cite journal |arxiv=1507.08532 |last1=Motalebi |first1=F. |display-authors=etal |title=The HARPS-N Rocky Planet Search. I. HD 219134 b: A transiting rocky planet in a multi-planet system at 6.5 pc from the Sun |date=December 2015 |doi=10.1051/0004-6361/201526822 |volume=584 |journal=] |page=A72 |bibcode=2015A&A...584A..72M |s2cid=45652878 }}</ref> |
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==Notes== |
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{{reflist|group=note}} |
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==External links== |
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==External links== |
A number of independent studies have been done regarding the planetary system of HD 219134, with some of their results conflicting with each other. As of March 2017, the star is known to have at least 5 planets, with two of them (HD 219134 b and c) known to be transiting, rocky super-Earths. The previously reported planets HD 219134 g and h were not reported in following HARPS-N analyses in March 2017 by Gillon et al.
Category
