| Revision as of 01:54, 23 May 2023 editCitation bot (talk | contribs)Bots5,406,790 edits Add: bibcode. | Use this bot. Report bugs. | Suggested by Headbomb | Linked from Misplaced Pages:WikiProject_Academic_Journals/Journals_cited_by_Wikipedia/Sandbox | #UCB_webform_linked 464/1208← Previous edit |
Latest revision as of 01:09, 23 September 2024 edit undo21.Andromedae (talk | contribs)Extended confirmed users, IP block exemptions8,211 editsNo edit summaryTags: Mobile edit Mobile web edit Advanced mobile edit |
| (9 intermediate revisions by 7 users not shown) |
| Line 40: |
Line 40: |
|
| mass = {{val|0.81|0.03}}<ref name=NASAExoplanetArchive/> |
|
| mass = {{val|0.81|0.03}}<ref name=NASAExoplanetArchive/> |
|
| gravity = {{val|4.567|0.018}}<ref name=NASAExoplanetArchive/> |
|
| gravity = {{val|4.567|0.018}}<ref name=NASAExoplanetArchive/> |
|
| radius = {{val|0.778|0.005}}<ref name=NASAExoplanetArchive/> |
|
| radius = {{val|0.7784|0.0053}}<ref name=Boyajian/> |
|
| rotational_velocity = 6.94<ref name=aaa520_A79/> |
|
| rotational_velocity = 6.94<ref name=aaa520_A79/> |
|
| luminosity =0.2646<ref name=NASAExoplanetArchive/> |
|
| luminosity ={{val|0.265|0.002}}<ref name=Boyajian/> |
|
| temperature = {{val|4699}}<ref name=NASAExoplanetArchive/> |
|
| temperature = {{val|4699|16|fmt=commas}}<ref name=Boyajian/> |
|
|
| habitable_inner = 0.467<ref name=Boyajian/> ] |
|
|
| habitable_outer = 0.926<ref name=Boyajian/> AU |
|
}} |
|
}} |
|
{{Starbox catalog |
|
{{Starbox catalog |
| Line 56: |
Line 58: |
|
|
|
|
|
== Planetary system == |
|
== Planetary system == |
|
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" /> |
|
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" /> |
|
|
|
|
|
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"/> |
|
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"/> |
| Line 104: |
Line 106: |
|
}} |
|
}} |
|
{{OrbitboxPlanet |
|
{{OrbitboxPlanet |
|
| exoplanet = ]<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 }}</ref> |
|
| 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> |
|
| mass_earth = >98 |
|
| mass_earth = >98 |
|
| period = {{val|2100.6|2.9}} |
|
| period = {{val|2100.6|2.9}} |
| Line 113: |
Line 115: |
|
|
|
|
|
=== Habitable Zone === |
|
=== Habitable Zone === |
|
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 }}</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. |
|
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. |
|
|
|
|
|
==References== |
|
==References== |
|
{{Reflist|refs= |
|
{{Reflist|refs= |
|
|
|
|
|
<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> |
|
|
|
|
|
<ref name="GaiaDR3">{{Cite Gaia DR3|2009481748875806976}}</ref> |
|
<ref name="GaiaDR3">{{Cite Gaia DR3|2009481748875806976}}</ref> |
| Line 131: |
Line 135: |
|
<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> |
|
<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> |
|
|
|
|
|
<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> |
|
<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> |
|
|
|
|
|
<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> |
|
<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> |
| Line 137: |
Line 141: |
|
<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> |
|
<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> |
|
|
|
|
|
<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> |
|
<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> |
|
|
|
|
|
<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> |
| Line 143: |
Line 147: |
|
<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> |
|
|
|
|
|
<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 }}</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 | issue=3 | 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> |
| Line 157: |
Line 161: |
|
| last12=Sinukoff | first12=Evan | last13=Macintosh | first13=Bruce |
|
| last12=Sinukoff | first12=Evan | last13=Macintosh | first13=Bruce |
|
| journal=] | year=2021 | volume=161 | issue=3 | page=134 | postscript=. |
|
| 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 }}</ref> |
|
| doi=10.3847/1538-3881/abd639 | arxiv=2012.09190 | bibcode=2021AJ....161..134H | s2cid=229297873 | doi-access=free }}</ref> |
|
|
|
|
|
<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}}</ref> |
|
<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> |
|
|
|
|
|
<ref name=SIMBAD>{{cite simbad | title=HR 8832 | access-date=2012-04-08 }}</ref> |
|
<ref name=SIMBAD>{{cite simbad | title=HR 8832 | access-date=2012-04-08 }}</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.
Category
