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{{Short description|Binary star system in the constellation of Andromeda}}
{{Sky|00|18|22.8850|+|44|01|22.6373|11.6}}
{{Starbox begin {{Starbox begin
| name = Groombridge 34 | name = Groombridge 34
}}
⚫ {{Starbox image
| image = ]
| caption = ] ]s for GX Andromedae, with flares marked by red arrows. Adapted from Pettersen and Griffin (1980)<ref name="Pettersen"/>
}} }}
{{Starbox observe 2s {{Starbox observe 2s
Line 6: Line 12:
| constell = ] | constell = ]
| component1 = Groombridge 34 A | component1 = Groombridge 34 A
| ra1 = {{RA|00|18|22.8850}}<ref name="Gaia DR2 A"/> | ra1 = {{RA|00|18|22.88498}}<ref name="Gaia DR3 A"/>
| dec1 = {{DEC|+44|01|22.6373}}<ref name="Gaia DR2 A"/> | dec1 = {{DEC|+44|01|22.6380}}<ref name="Gaia DR3 A"/>
| appmag_v1 = 8.119<ref name=apj804_1_64/> | appmag_v1 = 8.119<ref name=apj804_1_64/>
| component2 = Groombridge 34 B | component2 = Groombridge 34 B
| ra2 = {{RA|00|18|25.8244}}<ref name="Gaia DR2 B"/> | ra2 = {{RA|00|18|25.82514}}<ref name="Gaia DR3 B"/>
| dec2 = {{DEC|+44|01|38.0912}}<ref name="Gaia DR2 B"/> | dec2 = {{DEC|+44|01|38.0924}}<ref name="Gaia DR3 B"/>
| appmag_v2 = 11.007<ref name=apj804_1_64/> | appmag_v2 = 11.007<ref name=apj804_1_64/>
}} }}
Line 23: Line 29:
| component1 = Groombridge 34 A | component1 = Groombridge 34 A
| radial_v = {{Val|+11.62|0.08}}<ref name="Nidever2002"/> | radial_v = {{Val|+11.62|0.08}}<ref name="Nidever2002"/>
| prop_mo_ra = {{val|2891.525|0.061}}<ref name="Gaia DR2 A"/> | prop_mo_ra = {{val|2891.518|fmt=commas}}
| prop_mo_dec = {{val|411.903|0.034}}<ref name="Gaia DR2 A"/> | prop_mo_dec = {{val|411.832}}
| pm_footnote = <ref name="Gaia DR3 A"/>
| parallax = 280.6902 | parallax = 280.7068
| p_error = 0.0429 | p_error = 0.0203
| parallax_footnote = <ref name="Gaia DR2 A"/> | parallax_footnote = <ref name="Gaia DR3 A"/>
| absmag_v = | absmag_v = 10.32{{cn|date=November 2024}}
| component2 = Groombridge 34 B | component2 = Groombridge 34 B
| radial_v2 = | radial_v2 = {{val|10.60|0.15}}<ref name="Gaia DR3 B"/>
| prop_mo_ra2 = {{val|2863.284|0.069}}<ref name="Gaia DR2 B"/> | prop_mo_ra2 = {{val|2862.796|fmt=commas}}
| prop_mo_dec2 = {{val|336.529|0.039}}<ref name="Gaia DR2 B"/> | prop_mo_dec2 = {{val|336.432}}
| pm_footnote2 = <ref name="Gaia DR3 B"/>
| parallax2 = 280.7866 | parallax2 = 280.6947
| p_error2 = 0.0519 | p_error2 = 0.0278
| parallax_footnote2 = <ref name="Gaia DR2 B"/> | parallax_footnote2 = <ref name="Gaia DR3 B"/>
| absmag_v2 = | absmag_v2 = 13.3{{cn|date=November 2024}}
}} }}
{{Starbox visbin {{Starbox orbit
| reference = <ref name=lippincott1972/> | reference = <ref name=Pinamonti2018/>
| period = {{val|1230|930|110}}
⚫ | name=Groombridge 34 B
| axis_unitless = {{val|93|42|6|ul=AU}}
| period=2,600
⚫ | eccentricity = {{val|0.53|0.23|0.28}}
| axis=41.15
⚫ | inclination = {{val|54|11|16}}
⚫ | eccentricity=0.00
| node = {{val|2|35|43}}
⚫ | inclination=61.4
| periastron = {{val|7140|560|140}}
| node=45.3
}}
| periastron=1745
{{Starbox detail
}}<!--
⚫ -->{{Starbox detail
| component1 = Groombridge 34 A | component1 = Groombridge 34 A
| mass = {{val|0.38|0.05}}<ref name=Pinamonti2018/> | mass = {{val|0.393|0.009|0.008}}<ref name="Pineda2021"/>
| radius = {{val|0.38|0.05}}<ref name=Pinamonti2018/> | radius = {{val|0.385|0.002}}<ref name="Pineda2021"/>
| luminosity = ~0.022<ref name=Pinamonti2018/> | luminosity = 0.02249{{±|0.00019}}<ref name="Pineda2021"/>
| temperature = {{val|3,607|68}}<ref name=Pinamonti2018/> | temperature = {{val|3,601|12|11|fmt=commas}}<ref name="Pineda2021"/>
| gravity = {{val|4.87|0.04}}<ref name=Pinamonti2018/> | gravity = {{val|4.87|0.04}}<ref name=Pinamonti2018/>
| metal_fe = {{val|-0.34|0.09}}<ref name=Pinamonti2018/> | metal_fe = {{val|-0.34|0.09}}<ref name=Pinamonti2018/>
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}} }}
{{Starbox catalog {{Starbox catalog
| names=GX/GQ Andromedae, ]+43° 44, ] 49, ] 15 A/B, ] 171-047/171-048, ] 1326, ]&nbsp;1475, ] 3/4, LTT 10108/10109, ]&nbsp;36248.<ref name=SIMBAD/> | names=GX/GQ Andromedae, ]+43° 44, ] 49, ] 15 A/B, ] 171-047/171-048, ] 1326, ]&nbsp;1475, ] 3/4, LTT 10108/10109, ]&nbsp;36248, ]&nbsp;42798<ref name=SIMBAD/>
}} }}
{{Starbox reference {{Starbox reference
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| ARICNS = 00026 | an=GJ 15 A | ARICNS = 00026 | an=GJ 15 A
| ARICNS2 = 00027 | an2=GJ 15 B | ARICNS2 = 00027 | an2=GJ 15 B
}}
{{Starbox image
|image={{Location map|100x100|AlternativeMap=Andromeda_constellation_map.svg
|alt=Groombridge 34 is located in the constellation Andromeda.
|caption=Location of Groombridge 34 in the constellation ]|border=infobox|mark=Red_pog.png|width=325
⚫ |label=Groombridge&nbsp;34
|position=top
|lat=67.9
|long=70.7
}}|caption=
}} }}
{{Starbox end}} {{Starbox end}}
⚫ '''Groombridge 34''' is a binary star system in the northern ] of ]. It was listed as entry number 34 in ''A Catalogue of Circumpolar Stars'', published posthumously in 1838 by British astronomer ].<ref name=groombridge1838/> Based upon ] measurements taken by the ], the system is located about 11.6 light-years from the ]. This positions the pair among the ] to the Solar System.


⚫ '''Groombridge 34''' is a ] system in the northern ] of ]. It was listed as entry number 34 in ''A Catalogue of Circumpolar Stars'', published posthumously in 1838 by British astronomer ].<ref name=groombridge1838/> Based upon ] measurements taken by the ], the system is located about {{Convert|11.6|ly|pc|abbr=off|lk=on}} from the ]. This positions the pair among the ] to the Solar System.
⚫ Both components are small, dim ] stars that are too faint to be seen with the naked eye. They orbit around their common ] in a nearly circular orbit with a separation of about 147 ] and a ] of around 2,600&nbsp;years.<ref name=lippincott1972/> Both stars exhibit random variation in luminosity due to ] and they have been given ]s: the brighter member Groombridge 34 A is designated '''GX And''', while the smaller component is designated '''GQ And'''.<ref name=petit1990/>

⚫ Both components are small, dim ] stars that are too faint to be seen with the naked eye. They orbit around their common ] in a fairly ] orbit with a separation of about 93 ] and a ] of around 1,230&nbsp;years.<ref name=Pinamonti2018/> Both stars exhibit random variation in luminosity due to ] and they have been given ]s: the brighter member Groombridge 34 A is designated '''GX And''', while the smaller component is designated '''GQ And'''.<ref name=petit1990/>


The star system has a relatively high proper motion of 2.9&nbsp;]s per year,<ref name=aa575_A35/> and is moving away from the Solar System at a velocity of 11.6&nbsp;km/s.<ref name="Nidever2002"/> It achieved ] some 15,000 years ago when it came within {{Convert|3.5|pc|ly|abbr=on|lk=off|order=flip}} of the Sun.<ref name=aa575_A35/> The star system has a relatively high proper motion of 2.9&nbsp;]s per year,<ref name=aa575_A35/> and is moving away from the Solar System at a velocity of 11.6&nbsp;km/s.<ref name="Nidever2002"/> It achieved ] some 15,000 years ago when it came within {{cvt|3.5|pc|ly|order=flip}} of the Sun.<ref name=aa575_A35/>


==GX Andromedae== ==GX Andromedae==
The most massive and luminous component of the pair has the ] ''GX Andromedae''. It is a ] ] star of ] M1.4<ref name=apj804_1_64/> that varies his brightness due to ]s. ] observations suggest a rotation period of 44 days and a magnetic activity cycle of roughly 9 years.<ref name=Morris2018/> The more massive and luminous component of the pair has the ] ''GX Andromedae''. It is a ] ] star of ] M1.4<ref name=apj804_1_64/> that varies its brightness due to ]s. ] observations suggest a rotation period of 44 days and a magnetic activity cycle of roughly 9 years.<ref name=Morris2018/>


==GQ Andromedae== ==GQ Andromedae==
The smaller companion bears the variable star name ''GQ Andromedae''. It's a red dwarf main sequence star that undergoes flare events like the primary; it has a spectral type M4.1<ref name=apj804_1_64/>, so it has also a lower ]. The smaller companion bears the variable star name ''GQ Andromedae''. It is a red dwarf main sequence star that undergoes flare events like the primary; it has a spectral type M4.1,<ref name=apj804_1_64/> so it also has a lower ].


==Planetary system== ==Planetary system==
In August 2014, a planet orbiting around Groombridge 34 A was reported.<ref name=apj794_1_51/> The planet's existence was deduced from analysis of the ] of the parent Star by the Eta-Earth Survey using HIRES at ]. At the time of its discovery, it was the sixth-nearest known ]. In August 2014, a planet orbiting around Groombridge 34 A was reported.<ref name=apj794_1_51/> The planet's existence was deduced from analysis of the ] of the parent star by the Eta-Earth Survey using ] at ]. At the time of its discovery, it was the sixth-nearest-known ].


Using the ] spectrograph combined with the measurements of the HARPS and HIRES spectrographs, researchers failed to detect the purported Groombridge 34 Ab. However, they did propose another that another planet (Groombridge 34 Ac, GJ 15 Ac) could be orbiting the parent star.<ref name=Trifonov>{{cite journal|doi=10.1051/0004-6361/201731442|title=The CARMENES search for exoplanets around M dwarfs. First visual-channel radial-velocity measurements and orbital parameter updates of seven M-dwarf planetary systems|journal=Astronomy & Astrophysics|volume=609|pages=A117|year=2018|last1=Trifonov|first1=T|last2=Kürster|first2=M|last3=Zechmeister|first3=M|last4=Tal-Or|first4=L|last5=Caballero|first5=J|last6=Quirrenbach|first6=A|last7=Ribas|first7=I|last8=Reiners|first8=A|arxiv=1710.01595|bibcode=2018A&A...609A.117T|s2cid=119340839}}</ref> Using the ] spectrograph combined with the measurements of the ] and HIRES spectrographs, researchers failed to detect the purported Groombridge 34 Ab. However, they did propose that another planet (Groombridge 34 Ac, GJ 15 Ac) could be orbiting the parent star.<ref name=Trifonov>{{cite journal |doi=10.1051/0004-6361/201731442 |title=The CARMENES search for exoplanets around M dwarfs. First visual-channel radial-velocity measurements and orbital parameter updates of seven M-dwarf planetary systems |last1=Trifonov |first1=Trifon |last2=Kürster |first2=Martin |last3=Zechmeister |first3=Mathias |last4=Tal-Or |first4=Lev |last5=Caballero |first5=José A. |last6=Quirrenbach |first6=Andreas |last7=Amado |first7=Pedro J. |last8=Ribas |first8=Ignasi |last9=Reiners |first9=Ansgar |last10=Reffert |first10=Sabine |last11=Dreizler |first11=Stefan |last12=Hatzes |first12=Artie P. |last13=Kaminski |first13=Adrian |last14=Launhardt |first14=Ralf |last15=Henning |first15=Thomas K. |last16=Montes |first16=David |last17=Béjar |first17=Victor J. S. |last18=Mundt |first18=Reinhard |last19=Pavlov |first19=Aleksei |last20=Schmitt |first20=Jürgen H. M. M. |last21=Seifert |first21=Walter |last22=Morales |first22=Juan Carlos |last23=Nowak |first23=Grzegorz |last24=Jeffers |first24=Sandra V. |last25=Rodríguez-López |first25=Cristina |last26=del Burgo |first26=Carlos |last27=Anglada-Escudé |first27=Guillem |last28=López-Santiago |first28=Javier |last29=Mathar |first29=Richard J. |last30=Ammler-von Eiff |first30=Matthias <!-- over 100 more -->|display-authors=9 |journal=Astronomy and Astrophysics |volume=609 |at=A117 |year=2018 |arxiv=1710.01595 |bibcode=2018A&A...609A.117T |s2cid=119340839 }}</ref>


This discrepancy was later reconciled with new HIRES observations, covering a longer span of time, where both planets were recovered, constraining their minimum mass to 3.03 {{Earth mass|link=yes}} for Groombridge 34 Ab and 36 {{Earth mass}} for Groombridge Ac. Their orbital periods are 11.4 and approximately 7,600 days, respectively. To date, this is the fifth-closest multi-planet system to our ], hosting the longest period Neptune-mass exoplanet discovered so far.<ref name=Pinamonti2018/> This discrepancy was later reconciled with new HIRES observations, covering a longer span of time, where both planets were recovered, constraining their minimum mass to 3.03 {{Earth mass|link=yes}} for Groombridge 34 Ab and 36 {{Earth mass}} for Groombridge Ac. Their orbital periods are 11.4 and approximately 7,600 days, respectively. To date, this is the fourth-closest confirmed multi-planet system to the ], hosting the longest-period Neptune-mass exoplanet discovered so far.<ref name=Pinamonti2018/>


{{OrbitboxPlanet begin |name=Groombridge 34 A {{OrbitboxPlanet begin
| name = Groombridge 34 A
| table_ref = <ref name=Pinamonti2018/> | table_ref = <ref name=Pinamonti2018/>
}} }}
{{OrbitboxPlanet {{OrbitboxPlanet
| exoplanet = ] | exoplanet = ]
| mass_earth = ≥ {{val|3.03|0.46|0.44}} | mass_earth = {{val|3.03|0.46|0.44|p=≥}}
| period = {{val|11.4407|0.0017|0.0016}} | period = {{val|11.4407|0.0017|0.0016}}
| semimajor = {{val|0.072|0.003|0.004}} | semimajor = {{val|0.072|0.003|0.004}}
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}} }}
{{OrbitboxPlanet {{OrbitboxPlanet
| exoplanet = ] | exoplanet = ]
| mass_earth = ≥ {{val|36|25|18}} | mass_earth = {{val|36|25|18|p=≥}}
| period = ~7,600 | period = ~7,600
| semimajor = {{val|5.4|1.0|0.9}} | semimajor = {{val|5.4|1.0|0.9}}
Line 122: Line 141:


==See also== ==See also==
⚫ *]
*]
⚫ *]


==References== ==References==
{{Reflist|refs= {{Reflist|refs=


<ref name="Gaia DR2 A">{{cite DR2|385334230892516480}}</ref> <ref name="Gaia DR3 A">{{cite Gaia DR3|385334230892516480}}</ref>


<ref name="Gaia DR2 B">{{cite DR2|385334196532776576}}</ref> <ref name="Gaia DR3 B">{{cite Gaia DR3|385334196532776576}}</ref>

<ref name="Pineda2021">{{cite journal | title=The M-dwarf Ultraviolet Spectroscopic Sample. I. Determining Stellar Parameters for Field Stars | last1=Pineda | first1=J. Sebastian | last2=Youngblood | first2=Allison | last3=France | first3=Kevin | journal=The Astrophysical Journal | volume=918 | issue=1 | id=40 | pages=23 | date=September 2021 | doi=10.3847/1538-4357/ac0aea | arxiv=2106.07656 | bibcode=2021ApJ...918...40P | s2cid=235435757 | doi-access=free }}</ref>


<ref name=apj794_1_51>{{citation <ref name=apj794_1_51>{{citation
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| arxiv=1408.5645 | s2cid=17361592 | postscript=. | arxiv=1408.5645 | s2cid=17361592 | postscript=.
}}</ref> }}</ref>

<ref name="Pettersen">{{cite journal
| last1=Pettersen | first1=B. R. | last2=Griffin | first2=R. F.
| title=Non-emission-line flare stars | bibcode=1980Obs...100..198P
| journal=The Observatory | date=December 1980 | volume=100 | pages=198–202
| url=https://ui.adsabs.harvard.edu/abs/1980Obs...100..198P | access-date=30 October 2022}}</ref>


<ref name=apj804_1_64>{{citation <ref name=apj804_1_64>{{citation
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| postscript=. }}</ref> | postscript=. }}</ref>


<ref name=lippincott1972>{{citation <!--<ref name=lippincott1972>{{citation
| title=Parallax and orbital motion of the two nearby long period visual binaries Groombridge 34 and ADS 9090. | title=Parallax and orbital motion of the two nearby long period visual binaries Groombridge 34 and ADS 9090.
| last1=Lippincott | first1=S. L. | last1=Lippincott | first1=S. L.
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| doi=10.1086/111261 | doi=10.1086/111261
| bibcode=1972AJ.....77..165L | bibcode=1972AJ.....77..165L
| postscript=. }}</ref> | postscript=. }}</ref>-->


<ref name=petit1990>{{citation <ref name=petit1990>{{citation
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| bibcode=2013AJ....146...99C | arxiv=1307.7038 | s2cid=44208180 | postscript=. }}</ref> | bibcode=2013AJ....146...99C | arxiv=1307.7038 | s2cid=44208180 | postscript=. }}</ref>


<ref name=Morris2018>{{cite journal|bibcode=2018MNRAS.476.5408M|title=Spotting stellar activity cycles in Gaia astrometry|journal=Monthly Notices of the Royal Astronomical Society|volume=476|issue=4|pages=5408|last1=Morris|first1=Brett M.|last2=Agol|first2=Eric|last3=Davenport|first3=James R. A.|last4=Hawley|first4=Suzanne L.|year=2018|arxiv=1802.09943|doi=10.1093/mnras/sty568|s2cid=73564680}}</ref> <ref name=Morris2018>{{cite journal|bibcode=2018MNRAS.476.5408M|title=Spotting stellar activity cycles in Gaia astrometry|journal=Monthly Notices of the Royal Astronomical Society|volume=476|issue=4|pages=5408|last1=Morris|first1=Brett M.|last2=Agol|first2=Eric|last3=Davenport|first3=James R. A.|last4=Hawley|first4=Suzanne L.|year=2018|arxiv=1802.09943|doi=10.1093/mnras/sty568|doi-access=free |s2cid=73564680}}</ref>


<ref name=Pinamonti2018>{{cite journal|bibcode=2018A&A...617A.104P|title=The HADES RV Programme with HARPS-N at TNG. VIII. GJ15A: A multiple wide planetary system sculpted by binary interaction|journal=Astronomy and Astrophysics|volume=617|pages=A104|last1=Pinamonti|first1=M.|last2=Damasso|first2=M.|last3=Marzari|first3=F.|last4=Sozzetti|first4=A.|last5=Desidera|first5=S.|last6=Maldonado|first6=J.|last7=Scandariato|first7=G.|last8=Affer|first8=L.|last9=Lanza|first9=A. F.|last10=Bignamini|first10=A.|last11=Bonomo|first11=A. S.|last12=Borsa|first12=F.|last13=Claudi|first13=R.|last14=Cosentino|first14=R.|last15=Giacobbe|first15=P.|last16=González-Álvarez|first16=E.|last17=González Hernández|first17=J. I.|last18=Gratton|first18=R.|last19=Leto|first19=G.|last20=Malavolta|first20=L.|last21=Martinez Fiorenzano|first21=A.|last22=Micela|first22=G.|last23=Molinari|first23=E.|last24=Pagano|first24=I.|last25=Pedani|first25=M.|last26=Perger|first26=M.|last27=Piotto|first27=G.|last28=Rebolo|first28=R.|last29=Ribas|first29=I.|last30=Suárez Mascareño|first30=A.|displayauthors=29|year=2018|arxiv=1804.03476|doi=10.1051/0004-6361/201732535|s2cid=54990041}}</ref> <ref name=Pinamonti2018>{{cite journal|bibcode=2018A&A...617A.104P|title=The HADES RV Programme with HARPS-N at TNG. VIII. GJ15A: A multiple wide planetary system sculpted by binary interaction|journal=Astronomy and Astrophysics|volume=617|pages=A104|last1=Pinamonti|first1=M.|last2=Damasso|first2=M.|last3=Marzari|first3=F.|last4=Sozzetti|first4=A.|last5=Desidera|first5=S.|last6=Maldonado|first6=J.|last7=Scandariato|first7=G.|last8=Affer|first8=L.|last9=Lanza|first9=A. F.|last10=Bignamini|first10=A.|last11=Bonomo|first11=A. S.|last12=Borsa|first12=F.|last13=Claudi|first13=R.|last14=Cosentino|first14=R.|last15=Giacobbe|first15=P.|last16=González-Álvarez|first16=E.|last17=González Hernández|first17=J. I.|last18=Gratton|first18=R.|last19=Leto|first19=G.|last20=Malavolta|first20=L.|last21=Martinez Fiorenzano|first21=A.|last22=Micela|first22=G.|last23=Molinari|first23=E.|last24=Pagano|first24=I.|last25=Pedani|first25=M.|last26=Perger|first26=M.|last27=Piotto|first27=G.|last28=Rebolo|first28=R.|last29=Ribas|first29=I.|last30=Suárez Mascareño|first30=A.|display-authors=29|year=2018|arxiv=1804.03476|doi=10.1051/0004-6361/201732535|s2cid=54990041}}</ref>


}} }}
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==External links== ==External links==
* *
*
* *
*


{{nearest systems|3}} {{nearest systems|2}}
{{Stars of Andromeda}} {{Stars of Andromeda}}


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] ]
] ]
]
]

Latest revision as of 16:30, 2 November 2024

Binary star system in the constellation of Andromeda
Groombridge 34

Ultraviolet band light curves for GX Andromedae, with flares marked by red arrows. Adapted from Pettersen and Griffin (1980)
Observation data
Epoch J2000      Equinox J2000
Constellation Andromeda
Groombridge 34 A
Right ascension 00 18 22.88498
Declination +44° 01′ 22.6380″
Apparent magnitude (V) 8.119
Groombridge 34 B
Right ascension 00 18 25.82514
Declination +44° 01′ 38.0924″
Apparent magnitude (V) 11.007
Characteristics
Spectral type M1.4V + M4.1V
U−B color index +1.24/+1.40
B−V color index +1.56/+1.80
Variable type Flare stars
Astrometry
Groombridge 34 A
Radial velocity (Rv)+11.62±0.08 km/s
Proper motion (μ) RA: 2,891.518 mas/yr
Dec.: 411.832 mas/yr
Parallax (π)280.7068 ± 0.0203 mas
Distance11.6191 ± 0.0008 ly
(3.5624 ± 0.0003 pc)
Absolute magnitude (MV)10.32
Groombridge 34 B
Radial velocity (Rv)10.60±0.15 km/s
Proper motion (μ) RA: 2,862.796 mas/yr
Dec.: 336.432 mas/yr
Parallax (π)280.6947 ± 0.0278 mas
Distance11.620 ± 0.001 ly
(3.5626 ± 0.0004 pc)
Absolute magnitude (MV)13.3
Orbit
Period (P)1230+930
−110 yr
Semi-major axis (a)93+42
−6 AU
Eccentricity (e)0.53+0.23
−0.28
Inclination (i)54+11
−16°
Longitude of the node (Ω)2+35
−43°
Periastron epoch (T)7140+560
−140
Details
Groombridge 34 A
Mass0.393+0.009
−0.008 M☉
Radius0.385±0.002 R☉
Luminosity0.02249±0.00019 L☉
Habitable zone inner limit0.112 AU
Habitable zone outer limit0.239 AU
Surface gravity (log g)4.87±0.04 cgs
Temperature3,601+12
−11 K
Metallicity −0.34±0.09 dex
Rotation43.86±0.56 days
Rotational velocity (v sin i)1.09±0.79 km/s
Age~3.02 Gyr
Groombridge 34 B
Mass0.15±0.02 M☉
Radius0.18±0.03 R☉
Luminosity~8.5×10 L☉
Habitable zone inner limit0.048 AU
Habitable zone outer limit0.103 AU
Surface gravity (log g)5.08±0.15 cgs
Temperature3304±70 K
Metallicity −0.37±0.10 dex
Age~2.754 Gyr
Other designations
GX/GQ Andromedae, BD+43° 44, GCTP 49, GJ 15 A/B, G 171-047/171-048, HD 1326, HIP 1475, LHS 3/4, LTT 10108/10109, SAO 36248, PPM 42798
Database references
SIMBADGJ 15 A
GJ 15 Ab
GJ 15 B
ARICNSGJ 15 A
GJ 15 B
Groombridge 34 is located in the constellation Andromeda.Groombridge 34 is located in the constellation Andromeda.Groombridge 34Location of Groombridge 34 in the constellation Andromeda

Groombridge 34 is a binary star system in the northern constellation of Andromeda. It was listed as entry number 34 in A Catalogue of Circumpolar Stars, published posthumously in 1838 by British astronomer Stephen Groombridge. Based upon parallax measurements taken by the Gaia spacecraft, the system is located about 11.6 light-years (3.6 parsecs) from the Sun. This positions the pair among the nearest stars to the Solar System.

Both components are small, dim red dwarf stars that are too faint to be seen with the naked eye. They orbit around their common barycenter in a fairly eccentric orbit with a separation of about 93 AU and a period of around 1,230 years. Both stars exhibit random variation in luminosity due to flares and they have been given variable star designations: the brighter member Groombridge 34 A is designated GX And, while the smaller component is designated GQ And.

The star system has a relatively high proper motion of 2.9 arc seconds per year, and is moving away from the Solar System at a velocity of 11.6 km/s. It achieved perihelion some 15,000 years ago when it came within 11 ly (3.5 pc) of the Sun.

GX Andromedae

The more massive and luminous component of the pair has the variable star designation GX Andromedae. It is a main-sequence red dwarf star of spectral type M1.4 that varies its brightness due to stellar flares. Gaia observations suggest a rotation period of 44 days and a magnetic activity cycle of roughly 9 years.

GQ Andromedae

The smaller companion bears the variable star name GQ Andromedae. It is a red dwarf main sequence star that undergoes flare events like the primary; it has a spectral type M4.1, so it also has a lower effective temperature.

Planetary system

In August 2014, a planet orbiting around Groombridge 34 A was reported. The planet's existence was deduced from analysis of the radial velocities of the parent star by the Eta-Earth Survey using HIRES at Keck Observatory. At the time of its discovery, it was the sixth-nearest-known exoplanet.

Using the CARMENES spectrograph combined with the measurements of the HARPS and HIRES spectrographs, researchers failed to detect the purported Groombridge 34 Ab. However, they did propose that another planet (Groombridge 34 Ac, GJ 15 Ac) could be orbiting the parent star.

This discrepancy was later reconciled with new HIRES observations, covering a longer span of time, where both planets were recovered, constraining their minimum mass to 3.03 ME for Groombridge 34 Ab and 36 ME for Groombridge Ac. Their orbital periods are 11.4 and approximately 7,600 days, respectively. To date, this is the fourth-closest confirmed multi-planet system to the Sun, hosting the longest-period Neptune-mass exoplanet discovered so far.

The Groombridge 34 A planetary system
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b ≥3.03+0.46
−0.44 M🜨 		0.072+0.003
−0.004 		11.4407+0.0017
−0.0016 		0.094+0.091
−0.065 		— —
c ≥36+25
−18 M🜨 		5.4+1.0
−0.9 		~7,600 0.27+0.28
−0.19 		— —

See also

References

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  3. ^ Mann, Andrew W.; et al. (May 2015), "How to Constrain Your M Dwarf: Measuring Effective Temperature, Bolometric Luminosity, Mass, and Radius", The Astrophysical Journal, 804 (1): 38, arXiv:1501.01635, Bibcode:2015ApJ...804...64M, doi:10.1088/0004-637X/804/1/64, S2CID 19269312, 64.
  4. ^ Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  5. ^ Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data. SIMBAD, Bibcode:1986EgUBV........0M.
  6. ^ Nidever, David L.; et al. (August 2002), "Radial Velocities for 889 Late-Type Stars", The Astrophysical Journal Supplement Series, 141 (2): 503–522, arXiv:astro-ph/0112477, Bibcode:2002ApJS..141..503N, doi:10.1086/340570, S2CID 51814894.
  7. ^ Pinamonti, M.; Damasso, M.; Marzari, F.; Sozzetti, A.; Desidera, S.; Maldonado, J.; Scandariato, G.; Affer, L.; Lanza, A. F.; Bignamini, A.; Bonomo, A. S.; Borsa, F.; Claudi, R.; Cosentino, R.; Giacobbe, P.; González-Álvarez, E.; González Hernández, J. I.; Gratton, R.; Leto, G.; Malavolta, L.; Martinez Fiorenzano, A.; Micela, G.; Molinari, E.; Pagano, I.; Pedani, M.; Perger, M.; Piotto, G.; Rebolo, R.; Ribas, I.; et al. (2018). "The HADES RV Programme with HARPS-N at TNG. VIII. GJ15A: A multiple wide planetary system sculpted by binary interaction". Astronomy and Astrophysics. 617: A104. arXiv:1804.03476. Bibcode:2018A&A...617A.104P. doi:10.1051/0004-6361/201732535. S2CID 54990041.
  8. ^ Pineda, J. Sebastian; Youngblood, Allison; France, Kevin (September 2021). "The M-dwarf Ultraviolet Spectroscopic Sample. I. Determining Stellar Parameters for Field Stars". The Astrophysical Journal. 918 (1): 23. arXiv:2106.07656. Bibcode:2021ApJ...918...40P. doi:10.3847/1538-4357/ac0aea. S2CID 235435757. 40.
  9. ^ Cantrell, Justin R.; et al. (October 2013), "The Solar Neighborhood XXIX: The Habitable Real Estate of Our Nearest Stellar Neighbors", The Astronomical Journal, 146 (4): 99, arXiv:1307.7038, Bibcode:2013AJ....146...99C, doi:10.1088/0004-6256/146/4/99, S2CID 44208180.
  10. "V* GX And". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-02-09.{{cite web}}: CS1 maint: postscript (link)
  11. Groombridge, Stephen (1838), Airy, George Biddell (ed.), A Catalogue of Circumpolar Stars, J. Murray, p. 2.
  12. Petit, M. (October 1990), "Catalogue des étoiles variables ou suspectes dans le voisinage du Soleil", Astronomy and Astrophysics Supplement (in French), 85 (2): 971, Bibcode:1990A&AS...85..971P.
  13. ^ Bailer-Jones, C. A. L. (March 2015). "Close encounters of the stellar kind". Astronomy & Astrophysics. 575: 13. arXiv:1412.3648. Bibcode:2015A&A...575A..35B. doi:10.1051/0004-6361/201425221. S2CID 59039482. A35.
  14. Morris, Brett M.; Agol, Eric; Davenport, James R. A.; Hawley, Suzanne L. (2018). "Spotting stellar activity cycles in Gaia astrometry". Monthly Notices of the Royal Astronomical Society. 476 (4): 5408. arXiv:1802.09943. Bibcode:2018MNRAS.476.5408M. doi:10.1093/mnras/sty568. S2CID 73564680.
  15. Howard, Andrew W.; et al. (October 2014), "The NASA-UC-UH ETA-Earth Program. IV. A Low-mass Planet Orbiting an M Dwarf 3.6 PC from Earth", The Astrophysical Journal, 794 (1): 9, arXiv:1408.5645, Bibcode:2014ApJ...794...51H, doi:10.1088/0004-637X/794/1/51, S2CID 17361592, 51.
  16. Trifonov, Trifon; Kürster, Martin; Zechmeister, Mathias; Tal-Or, Lev; Caballero, José A.; Quirrenbach, Andreas; Amado, Pedro J.; Ribas, Ignasi; Reiners, Ansgar; et al. (2018). "The CARMENES search for exoplanets around M dwarfs. First visual-channel radial-velocity measurements and orbital parameter updates of seven M-dwarf planetary systems". Astronomy and Astrophysics. 609. A117. arXiv:1710.01595. Bibcode:2018A&A...609A.117T. doi:10.1051/0004-6361/201731442. S2CID 119340839.

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