| Revision as of 02:02, 14 December 2021 edit86.169.130.101 (talk) →Habitable Zone← Previous edit |
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{{short description|Main-sequence star in the constellation Cassiopeia}} |
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{{short description|Star in the constellation Cassiopeia}} |
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{{Starbox begin |
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{{Starbox begin |
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| name = HD 219134 |
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| name = HD 219134 |
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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}} |
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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}} |
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| pm_footnote = <ref name="GaiaDR3"/> |
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| parallax = 152.76 |
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| p_error = 0.29 |
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| parallax = 152.8640 |
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| p_error = 0.0494 |
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| parallax_footnote = <ref name=aaa474_2_653/> |
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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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}} |
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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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}} |
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}} |
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{{Starbox catalog |
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{{Starbox catalog |
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| names = ]+56 2966, ] 875, ] 5616.00, ] 892, ] 219134, ] 114622, ] 1767, ] 71, ] 16826, ] 35236.<ref name=SIMBAD/> |
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| names = ]+56 2966, ] 875, ] 5616.00, ] 892, ] 219134, ] 114622, ] 8832, ] 1767, ] 71, ] 16826, ] 35236.<ref name=SIMBAD/> |
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{{Starbox reference |
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{{Starbox reference |
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{{Starbox end}} |
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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 our ], 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 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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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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{{OrbitboxPlanet begin |
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{{OrbitboxPlanet begin |
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{{OrbitboxPlanet |
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{{OrbitboxPlanet |
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| exoplanet = ] (e)<ref>{{citation|arxiv=2209.06958|year=2023|title=TESS-Keck Survey. XIV. Two Giant Exoplanets from the Distant Giants Survey|doi=10.3847/1538-3881/aca6ef |last1=Van Zandt |first1=Judah |last2=Petigura |first2=Erik A. |last3=MacDougall |first3=Mason |last4=Gilbert |first4=Gregory J. |last5=Lubin |first5=Jack |last6=Barclay |first6=Thomas |last7=Batalha |first7=Natalie M. |last8=Crossfield |first8=Ian J. M. |last9=Dressing |first9=Courtney |last10=Fulton |first10=Benjamin |last11=Howard |first11=Andrew W. |last12=Huber |first12=Daniel |last13=Isaacson |first13=Howard |last14=Kane |first14=Stephen R. |last15=Robertson |first15=Paul |last16=Roy |first16=Arpita |last17=Weiss |first17=Lauren M. |last18=Behmard |first18=Aida |last19=Beard |first19=Corey |last20=Chontos |first20=Ashley |last21=Dai |first21=Fei |last22=Dalba |first22=Paul A. |last23=Fetherolf |first23=Tara |last24=Giacalone |first24=Steven |last25=Henze |first25=Christopher E. |last26=Hill |first26=Michelle L. |last27=Hirsch |first27=Lea A. |last28=Holcomb |first28=Rae |last29=Howell |first29=Steve B. |last30=Jenkins |first30=Jon M. |journal=The Astronomical Journal |volume=165 |issue=2 |page=60 |bibcode=2023AJ....165...60V |s2cid=252280288 |display-authors=1 |doi-access=free }}</ref> |
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| exoplanet = ] |
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| mass_earth = >{{val|108|6}} |
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| mass_earth = >98 |
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| period = {{val|2247|43}} |
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| period = {{val|2100.6|2.9}} |
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| semimajor = {{val|3.11|0.04}} |
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| semimajor = {{val|3.11|0.04}} |
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| eccentricity = {{val|0.06|0.04}} |
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| eccentricity = {{val|0.06|0.04}} |
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=== Habitable Zone === |
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=== Habitable Zone === |
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The ] (CHZ) of HD 219134 is predicted 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}}</ref> None of the planets found orbiting the star are inside this habitable zone, although the unconfirmed ] orbits closest to it, but slightly interior to the inner edge of the optimistic habitable zone (OHZ), or recent Venus as it is sometimes described, which lies at 0.408 AU.<ref name="exoplanetkyoto"/> The planet also appears to be significantly more massive than Earth and therefore it likely retains a dense atmosphere. It is probably tidally locked with as yet no planetary mass satellites discovered in orbit around it. |
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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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==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=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=aaa172_235>{{citation | last=Perrin | first=M.-N. | last2=Karoji | first2=H. | title=Stellar radius determination from IRAS 12-micron fluxes | journal=Astronomy and Astrophysics | year=1987 | volume=172 | pages=235–240 | bibcode=1987A&A...172..235P | postscript=. }}</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=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 | access-date=2018-11-04 | archive-date=2017-09-22 | archive-url=https://web.archive.org/web/20170922031257/http://eprints.ucm.es/37826/1/davidmontes17libre.pdf | url-status=dead }}</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=aaass65_2_405>{{citation | last1=Oja | first1=T. | title=UBV photometry of stars whose positions are accurately known. III | journal=Astronomy and Astrophysics Supplement Series | volume=65 | issue=2 | pages=405–409 |date=August 1986 | bibcode=1986A&AS...65..405O | postscript=. }}</ref> |
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<ref name=aaass65_2_405>{{citation | last1=Oja | first1=T. | title=UBV photometry of stars whose positions are accurately known. III | journal=Astronomy and Astrophysics Supplement Series | volume=65 | issue=2 | pages=405–409 |date=August 1986 | bibcode=1986A&AS...65..405O | postscript=. }}</ref> |
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<ref name=csvs>{{citation | display-authors=1 | last1=Kukarkin | first1=B. V. | last2=Kholopov | first2=P. N. | last3=Artiukhina | first3=N. M. | last4=Fedorovich | first4=V. P. | last5=Frolov | first5=M. S. | last6=Goranskij | first6=V. P. | last7=Gorynya | first7=N. A. | last8=Karitskaya | first8=E. A. | last9=Kireeva | first9=N. N. | last10=Kukarkina | first10=N. P. | last11=Kurochkin | first11=N. E. | last12=Medvedeva | first12=G. I. | last13=Perova | first13=N. B. | last14=Ponomareva | first14=G. A. | last15=Samus | first15=N. N. | last16=Shugarov | first16=S. Y. | title=Nachrichtenblatt der Vereinigung der Sternfreunde e.V. (Catalogue of suspected variable stars) | journal=Nachrichtenblatt der Vereinigung der Sternfreunde E.V. (1981) | pages=0 | location=Moscow | publisher=Academy of Sciences USSR Shternberg | year=1981 | bibcode=1981CSV...C......0K | postscript=. }}</ref> |
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<ref name=csvs>{{citation | display-authors=1 | last1=Kukarkin | first1=B. V. | last2=Kholopov | first2=P. N. | last3=Artiukhina | first3=N. M. | last4=Fedorovich | first4=V. P. | last5=Frolov | first5=M. S. | last6=Goranskij | first6=V. P. | last7=Gorynya | first7=N. A. | last8=Karitskaya | first8=E. A. | last9=Kireeva | first9=N. N. | last10=Kukarkina | first10=N. P. | last11=Kurochkin | first11=N. E. | last12=Medvedeva | first12=G. I. | last13=Perova | first13=N. B. | last14=Ponomareva | first14=G. A. | last15=Samus | first15=N. N. | last16=Shugarov | first16=S. Y. | title=Nachrichtenblatt der Vereinigung der Sternfreunde e.V. (Catalogue of suspected variable stars) | journal=Nachrichtenblatt der Vereinigung der Sternfreunde E.V. (1981) | pages=0 | location=Moscow | publisher=Academy of Sciences USSR Shternberg | year=1981 | bibcode=1981CSV...C......0K | postscript=. }}</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 | doi-access=free | 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> |
|
<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="Vogt2015">{{cite journal |arxiv=1509.07912 |last1=Vogt |first1=Steven S. |display-authors=etal |title=Six Planets Orbiting HD 219134 |date=November 2015 |doi=10.1088/0004-637X/814/1/12 |volume=814 |issue=1 |journal=] |page=12 |bibcode=2015ApJ...814...12V|s2cid=45438051 }}</ref> |
|
<ref name="Vogt2015">{{cite journal |arxiv=1509.07912 |last1=Vogt |first1=Steven S. |display-authors=etal |title=Six Planets Orbiting HD 219134 |date=November 2015 |doi=10.1088/0004-637X/814/1/12 |volume=814 |issue=1 |journal=] |page=12 |bibcode=2015ApJ...814...12V|s2cid=45438051 }}</ref> |
|
|
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<ref name="Johnson2016">{{cite journal |arxiv=1602.05200 |last1=Johnson |first1=Marshall C. |display-authors=etal |title=A 12-year Activity Cycle for the Nearby Planet Host Star HD 219134 |date=April 2016 |doi=10.3847/0004-637X/821/2/74 |volume=821 |issue=2 |journal=] |page=74 |bibcode=2016ApJ...821...74J}}</ref> |
|
<ref name="Johnson2016">{{cite journal |arxiv=1602.05200 |last1=Johnson |first1=Marshall C. |display-authors=etal |title=A 12-year Activity Cycle for the Nearby Planet Host Star HD 219134 |date=April 2016 |doi=10.3847/0004-637X/821/2/74 |volume=821 |issue=2 |journal=] |page=74 |bibcode=2016ApJ...821...74J|s2cid=118651905 |doi-access=free }}</ref> |
|
|
|
|
|
<ref name="Gillon2017">{{cite journal | title=Two massive rocky planets transiting a K-dwarf 6.5 parsecs away | last1=Gillon | first1=Michaël | last2=Demory | first2=Brice-Olivier | last3=Grootel | first3=Valérie | last4=Motalebi | first4=Fatemeh | last5=Lovis | first5=Christophe | last6=Cameron | first6=Andrew | last7=Charbonneau | first7=David | last8=Latham | first8=David | last9=Molinari | first9=Emilio | last10=Pepe | first10=Francesco | last11=Ségransan | first11=Damien | last12=Sasselov | first12=Dimitar | last13=Udry | first13=Stéphane | last14=Mayor | first14=Michel | last15=Micela | first15=Giuseppina | last16=Piotto | first16=Giampaolo | last17=Sozzetti | first17=Alessandro | display-authors=1 | journal=Nature Astronomy | volume=1 | at=0056 | year=2017 | arxiv=1703.01430 | doi=10.1038/s41550-017-0056 | bibcode=2017NatAs...1E..56G | s2cid=56075932 }}</ref> |
|
<ref name="Gillon2017">{{cite journal | title=Two massive rocky planets transiting a K-dwarf 6.5 parsecs away | last1=Gillon | first1=Michaël | last2=Demory | first2=Brice-Olivier | last3=Grootel | first3=Valérie | last4=Motalebi | first4=Fatemeh | last5=Lovis | first5=Christophe | last6=Cameron | first6=Andrew | last7=Charbonneau | first7=David | last8=Latham | first8=David | last9=Molinari | first9=Emilio | last10=Pepe | first10=Francesco | last11=Ségransan | first11=Damien | last12=Sasselov | first12=Dimitar | last13=Udry | first13=Stéphane | last14=Mayor | first14=Michel | last15=Micela | first15=Giuseppina | last16=Piotto | first16=Giampaolo | last17=Sozzetti | first17=Alessandro | display-authors=1 | journal=Nature Astronomy | volume=1 | at=0056 | year=2017 | issue=3 | arxiv=1703.01430 | doi=10.1038/s41550-017-0056 | bibcode=2017NatAs...1E..56G | s2cid=56075932 }}</ref> |
|
|
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|
<ref name="Hirsch2020">{{citation |
|
|
|title=Understanding the Impacts of Stellar Companions on Planet Formation and Evolution: A Survey of Stellar and Planetary Companions within 25 pc |
|
|
| display-authors=1 | last1=Hirsch | first1=Lea A. |
|
|
| last2=Rosenthal | first2=Lee | last3=Fulton | first3=Benjamin J. |
|
|
| last4=Howard | first4=Andrew W. | last5=Ciardi | first5=David R. |
|
|
| last6=Marcy | first6=Geoffrey W. | last7=Nielsen | first7=Eric L. |
|
|
| last8=Petigura | first8=Erik A. | last9=de Rosa | first9=Robert J. |
|
|
| last10=Isaacson | first10=Howard | last11=Weiss | first11=Lauren M. |
|
|
| last12=Sinukoff | first12=Evan | last13=Macintosh | first13=Bruce |
|
|
| journal=] | year=2021 | volume=161 | issue=3 | page=134 | postscript=. |
|
|
| doi=10.3847/1538-3881/abd639 | arxiv=2012.09190 | bibcode=2021AJ....161..134H | s2cid=229297873 | doi-access=free }}</ref> |
|
|
|
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<ref name="Rosenthal2021">{{cite journal |arxiv=2105.11583|doi=10.3847/1538-4365/abe23c|title=The California Legacy Survey. I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades|year=2021|last1=Rosenthal|first1=Lee J.|last2=Fulton|first2=Benjamin J.|last3=Hirsch|first3=Lea A.|last4=Isaacson|first4=Howard T.|last5=Howard|first5=Andrew W.|last6=Dedrick|first6=Cayla M.|last7=Sherstyuk|first7=Ilya A.|last8=Blunt|first8=Sarah C.|last9=Petigura|first9=Erik A.|last10=Knutson|first10=Heather A.|last11=Behmard|first11=Aida|last12=Chontos|first12=Ashley|last13=Crepp|first13=Justin R.|last14=Crossfield|first14=Ian J. M.|last15=Dalba|first15=Paul A.|last16=Fischer|first16=Debra A.|last17=Henry|first17=Gregory W.|last18=Kane|first18=Stephen R.|last19=Kosiarek|first19=Molly|last20=Marcy|first20=Geoffrey W.|last21=Rubenzahl|first21=Ryan A.|last22=Weiss|first22=Lauren M.|last23=Wright|first23=Jason T. |display-authors=1 |journal=The Astrophysical Journal Supplement Series|volume=255|issue=1|page=8|bibcode=2021ApJS..255....8R|s2cid=235186973 |doi-access=free }}</ref> |
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<ref name=SIMBAD>{{cite simbad | title=HR 8832 | access-date=2012-04-08 }}</ref> |
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<ref name=SIMBAD>{{cite simbad | title=HR 8832 | access-date=2012-04-08 }}</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== |
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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. 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.
Category
