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| mass = {{val|0.81|0.03}}<ref name=NASAExoplanetArchive/> |
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| mass = {{val|0.81|0.03}}<ref name=NASAExoplanetArchive/> |
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| gravity = {{val|4.567|0.018}}<ref name=NASAExoplanetArchive/> |
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| gravity = {{val|4.567|0.018}}<ref name=NASAExoplanetArchive/> |
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| radius = {{val|0.778|0.005}}<ref name=NASAExoplanetArchive/> |
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| radius = {{val|0.7784|0.0053}}<ref name=Boyajian/> |
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| rotational_velocity = 6.94<ref name=aaa520_A79/> |
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| rotational_velocity = 6.94<ref name=aaa520_A79/> |
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| luminosity =0.2646<ref name=NASAExoplanetArchive/> |
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| luminosity ={{val|0.265|0.002}}<ref name=Boyajian/> |
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| temperature = {{val|4699}}<ref name=NASAExoplanetArchive/> |
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| temperature = {{val|4699|16|fmt=commas}}<ref name=Boyajian/> |
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| habitable_inner = 0.467<ref name=Boyajian/> ] |
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| habitable_outer = 0.926<ref name=Boyajian/> AU |
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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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'''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 ], 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 six known ]s. The innermost planet, ], is a rocky ] based on size (1.6 Earth radii), 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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HD 219134 has a system of six known ]s. The innermost planet, ], is a rocky ] based on size (1.6 Earth radii), 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 ] 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, ] ''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.<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> While a 2016 study suggested that the radial velocity signal corresponding to planet ''f'' might be caused by stellar activity,<ref name="Johnson2016" /> it has been confirmed by subsequent studies in 2017<ref name="Gillon2017" /> and 2021.<ref name="Rosenthal2021"/> Planet ''g'' has not been reported by subsequent studies, and a 2020 study did not find evidence of its claimed 94-day period, but instead found a period of 192 days.<ref name="Hirsch2020"/> |
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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.<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> While a 2016 study suggested that the radial velocity signal corresponding to planet ''f'' might be caused by stellar activity,<ref name="Johnson2016" /> it has been confirmed by subsequent studies in 2017<ref name="Gillon2017" /> and 2021.<ref name="Rosenthal2021"/> Planet ''g'' has not been reported by subsequent studies, and a 2020 study did not find evidence of its claimed 94-day period, but instead found a period of 192 days.<ref name="Hirsch2020"/> |
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=== Habitable Zone === |
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=== Habitable zone === |
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The ] (CHZ) of HD 219134 is estimated to extend from 0.516 to 0.948 AU.<ref name="exoplanetkyoto">{{Cite web|url=http://www.exoplanetkyoto.org/exohtml/HD_219134_g.html|title=HD 219134 g|publisher=]}}</ref><ref>{{cite web |url=http://hzgallery.org/1356_2.png |title=HD 219134 |website=hzgallery.org}}</ref> None of the planets orbiting the star are confirmed to orbit inside the habitable zone.<ref name="Dietrich2021">{{cite journal |author-link= |arxiv=2112.05337 |title= An Integrative Analysis of the HD 219134 Planetary System and the Inner solar system: Extending DYNAMITE with Enhanced Orbital Dynamical Stability Criteria|last1= Dietrich|first1= Jeremy|last2= Apai|first2= Dániel|last3= Malhotra|first3= Renu|journal=The Astronomical Journal |year= 2022|volume=163 |issue=2 |page=88 |doi=10.3847/1538-3881/ac4166 |bibcode=2022AJ....163...88D |s2cid=245117944 |doi-access=free }}</ref> The planet candidate ] may orbit slightly interior to the inner edge of the habitable zone based on its initially published parameters,<ref name="Vogt2015" /> or may orbit within the habitable zone based on a more recent estimated orbital period of 192 days and semi-major axis of 0.603 AU.<ref name="Hirsch2020"/> This planet is significantly more massive than Earth and therefore it likely retains a dense atmosphere, comparable to the Solar System's ]s. |
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The ] (CHZ) of HD 219134 is estimated to extend from 0.516 to 0.948 AU.<ref name="exoplanetkyoto">{{Cite web|url=http://www.exoplanetkyoto.org/exohtml/HD_219134_g.html|title=HD 219134 g|publisher=]}}</ref><ref>{{cite web |url=http://hzgallery.org/1356_2.png |title=HD 219134 |website=hzgallery.org}}</ref> As of 2024, none of the planets orbiting the star are confirmed to orbit inside the habitable zone.<ref name="Dietrich2021">{{cite journal |author-link= |arxiv=2112.05337 |title= An Integrative Analysis of the HD 219134 Planetary System and the Inner solar system: Extending DYNAMITE with Enhanced Orbital Dynamical Stability Criteria|last1= Dietrich|first1= Jeremy|last2= Apai|first2= Dániel|last3= Malhotra|first3= Renu|journal=The Astronomical Journal |year= 2022|volume=163 |issue=2 |page=88 |doi=10.3847/1538-3881/ac4166 |bibcode=2022AJ....163...88D |s2cid=245117944 |doi-access=free }}</ref> The planet candidate ] may orbit slightly interior to the inner edge of the habitable zone based on its initially published parameters,<ref name="Vogt2015" /> or may orbit within the habitable zone based on a more recent estimated orbital period of 192 days and semi-major axis of 0.603 AU.<ref name="Hirsch2020"/> This planet is significantly more massive than Earth and therefore it likely retains a dense atmosphere, comparable to the Solar System's ]s (see ]). |
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==References== |
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==References== |
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{{Reflist|refs= |
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<ref name=Boyajian>{{Cite journal |last=Boyajian |first=Tabetha S. |last2=von Braun |first2=Kaspar |last3=van Belle |first3=Gerard |last4=McAlister |first4=Harold A. |last5=Brummelaar |first5=Theo A. ten |last6=Kane |first6=Stephen R. |last7=Muirhead |first7=Phil |last8=Jones |first8=Jeremy |last9=White |first9=Russel |last10=Schaefer |first10=Gail |last11=Ciardi |first11=David |last12=Henry |first12=Todd |last13=López-Morales |first13=Mercedes |last14=Ridgway |first14=Stephen |last15=Gies |first15=Douglas |date=2012-10-01 |title=Stellar Diameters and Temperatures II. Main Sequence K & M Stars |arxiv=1208.2431 |journal=The Astrophysical Journal |volume=757 |issue=2 |pages=112 |doi=10.1088/0004-637X/757/2/112 |issn=0004-637X}}</ref> |
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<ref name="GaiaDR3">{{Cite Gaia DR3|2009481748875806976}}</ref> |
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<ref name="GaiaDR3">{{Cite Gaia DR3|2009481748875806976}}</ref> |
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. While a 2016 study suggested that the radial velocity signal corresponding to planet f might be caused by stellar activity, it has been confirmed by subsequent studies in 2017 and 2021. Planet g has not been reported by subsequent studies, and a 2020 study did not find evidence of its claimed 94-day period, but instead found a period of 192 days.
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