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{{Short description|Red dwarf star}}
{{Proposed deletion/dated
{{Starbox begin}}
|concern = Doesn't meet ]. None of the criteria are met.
{{Starbox image
|timestamp = 20150318150953
| image = ]
| caption = Artist's impression of GJ 1151 and an orbiting planet
}} }}
{{Starbox observe
'''GJ 1151''' is a ] star of ] M4.5V, located in constellation {{constel|UMa}} at 26.7 ]s from Earth.{{r|van Altena1995}}
| epoch = ]
| constell = ]
| ra = {{RA|11|50|57.72053}}<ref name=GaiaDR3/>
| dec = {{DEC|+48|22|38.5612}}<ref name=GaiaDR3/>
| appmag_v = 14.008<ref name=Houdebine2019/>
}}
{{Starbox character
| type =
| class = dM4.5<ref name=Houdebine2019/>
| b-v = 1.787<ref name=Mann2015/>
| u-b =
| variable =
}}
{{Starbox astrometry
| radial_v = {{val|−36.13|0.26}}<ref name=GaiaDR3/>
| prop_mo_ra = -1545.069
| prop_mo_dec = -962.724
| pm_footnote = <ref name=GaiaDR3/>
| parallax = 124.3378
| p_error = 0.0549
| parallax_footnote = <ref name=GaiaDR3/>
| absmag_v = {{Val|14.482|0.022}}<ref name=Houdebine2019/>
}}
{{Starbox detail
| source =
| mass = {{val|0.1639|0.0093}}<ref name="Blanco-Pozo2023"/>
| radius = {{val|0.1781|0.0042}}<ref name="Blanco-Pozo2023"/>
| luminosity_bolometric = {{val|0.003315|0.000018}}<ref name="Blanco-Pozo2023"/>
| temperature = {{Val|3143|26|fmt=commas}}<ref name=Houdebine2019/>
| gravity = {{val|5.09|0.09}}<ref name="Blanco-Pozo2023"/>
| metal_fe = {{val|-0.12|0.10}}<ref name="Blanco-Pozo2023"/>
| rotation = {{val|140|10|ul=d}}
| rotational_velocity = 2.0<ref name=Jeffers2018/>
| age_gyr = 2.5<ref name=Mann2015/>
}}
{{Starbox catalog
| names = {{odlist | GJ=1151 | LHS=316 | NLTT=28752 | G=122-49|2MASS=J11505787+4822395}}, Gaia EDR3 786834302080370304<ref name=SIMBAD/>
}}
{{Starbox reference
| Simbad = G+122-49
}}
{{Starbox end}}


'''GJ 1151''' is a ] located in the northern ] of ] at a distance of {{convert|26.2|ly|pc|lk=on|abbr=off}} from the ]. It has a reddish hue and is too faint to be visible to the naked eye with an ] of 14.0<ref name=Houdebine2019/> The star is moving closer with a ] of −36&nbsp;km/s,<ref name=Jeffers2018/> and has a relatively large ], traversing the ] at a rate of {{Val|1.815|ul=arcsecond}}·yr<sup>−1</sup>.<ref name=Lepine2005/>
==Distance==

{{πt}}
This is a small ] star of ] dM4.5.<ref name=Houdebine2019/> It is 2.5<ref name=Mann2015/>&nbsp;billion years old and is spinning with a ] of 2.0&nbsp;km/s.<ref name=Jeffers2018/> The star has 15.4%<ref name=Mann2015/> of the ] and 19.0%<ref name=Mann2015/> of the ], with an ] of 3,143&nbsp;K.<ref name=Houdebine2019/>
{{πp|gj|121.8|3.0|<ref name="Gliese1991">{{plxref|gj=1151}}</ref>}}

{{πp|plx|122.1|2.9|<ref name="van Altena1995">{{plxref|plx=2739.01}}</ref>|b=}}
==Planetary system==
{{πp|Dittmann ''et al.'' (2014)|130.60|3.60|{{r|Dittmann2014}}}}
In 2020, astronomers announced the discovery of radio emissions from the star which are consistent with the star having a magnetic interaction with a planet approximately the size of ], revolving in a 1-5 day long orbit.<ref name=Vedantham2020/><ref name="APJ-20200217"/><ref name="SA-20200229"/><ref name=SciNews/><ref name=Redd2020/><ref name=Clark/> Such an interaction would be analogous to a scaled-up version of the ], with GJ 1151 taking the role of Jupiter and its planet the role of Io.
{{πe}}

Two papers published only a month apart in 2021 discussed planet detection at GJ 1151 by the ]. One claimed the detection of a planet with a ] of {{Earth mass|2.5|link=y}} and a period of 2 days, supporting the radio emission detection,<ref name=Mahadevan2021/> while the other was unable to confirm this candidate planet, finding that the 2-day signal is likely caused by long-term variability, possibly connected to a more distant planet.<ref name=Perger2021/> This second study placed an upper limit of {{Earth mass|0.7-1.2}} on the minimum masses of any undetected planets with periods from 1-5 days.<ref name=Perger2021/>

In 2023, a different planet was found, with a minimum mass of {{Earth mass|10.6}} and a 390-day orbit, along with additional radial velocity variations. This new planet was referred to by the ] version of the discovery paper as GJ 1151 b, but the published version of the paper, as well as the ], refer to it as GJ 1151 c to differentiate it from the previous candidate. While the presence of a short-period planet associated with the radio emissions could not be completely ruled out, if such a planet exists its minimum mass must be less than {{Earth mass|1.2}}.<ref name="Blanco-Pozo2023"/>

{{OrbitboxPlanet begin
| name = GJ 1151
| table_ref = <ref name="Blanco-Pozo2023"/>
| period_unit = day
}}
{{OrbitboxPlanet
| exoplanet = c
| mass_earth = {{val|10.62|1.31|1.47|p=≥}}
| radius_earth =
| semimajor = {{val|0.5714|0.0053|0.0064}}
| period = {{val|389.7|5.4|6.5}}
| eccentricity =
| inclination =
}}
{{Orbitbox end}}

==See also==
*]


==References== ==References==
{{reflist|refs= {{reflist|refs=

<ref name="Dittmann2014">{{cite doi|10.1088/0004-637X/784/2/156}}</ref>
<ref name=GaiaDR3>{{Cite Gaia DR3|786834302080370304}}</ref>

<ref name=SIMBAD>{{cite simbad | title=G 122-49 | access-date=2020-03-02}}</ref>

<ref name=Lepine2005>{{cite journal
| last1=Lépine | first1=Sébastien | last2=Shara | first2=Michael M.
| title=A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)
| journal=The Astronomical Journal
| volume=129 | issue=3 | pages=1483–1522 | date=March 2005
| doi=10.1086/427854 | arxiv=astro-ph/0412070
| bibcode=2005AJ....129.1483L | s2cid=2603568 }}</ref>

<ref name=Mann2015>{{cite journal
| title=How to Constrain Your M Dwarf: Measuring Effective Temperature, Bolometric Luminosity, Mass, and Radius
| display-authors=1 | last1=Mann | first1=Andrew W.
| last2=Feiden | first2=Gregory A. | last3=Gaidos | first3=Eric
| last4=Boyajian | first4=Tabetha | last5=von Braun | first5=Kaspar
| journal=The Astrophysical Journal
| volume=804 | issue=1 | id=64 | pages=38 | date=May 2015
| arxiv=1501.01635 | bibcode=2015ApJ...804...64M
| doi=10.1088/0004-637X/804/1/64 | s2cid=19269312 }}</ref>

<ref name=Houdebine2019>{{cite journal
| title=The Mass-Activity Relationships in M and K Dwarfs. I. Stellar Parameters of Our Sample of M and K Dwarfs
| last1=Houdebine | first1=Éric R. | last2=Mullan | first2=D. J.
| last3=Doyle | first3=J. G. | last4=de La Vieuville | first4=Geoffroy
| last5=Butler | first5=C. J. | last6=Paletou | first6=F.
| display-authors=1 | journal=The Astronomical Journal
| volume=158 | issue=2 | id=56 | pages=17 | date=August 2019
| arxiv=1905.07921 | bibcode=2019AJ....158...56H
| doi=10.3847/1538-3881/ab23fe | s2cid=159041104 | doi-access=free }}</ref>

<ref name=Jeffers2018>{{cite journal
| title=CARMENES input catalogue of M dwarfs. III. Rotation and activity from high-resolution spectroscopic observations
| last1=Jeffers | first1=S. V. | last2=Schöfer | first2=P.
| last3=Lamert | first3=A. | last4=Reiners | first4=A.
| last5=Montes | first5=D. | last6=Caballero | first6=J. A.
| last7=Cortés-Contreras | first7=M. | last8=Marvin | first8=C. J.
| last9=Passegger | first9=V. M. | last10=Zechmeister | first10=M.
| last11=Quirrenbach | first11=A. | last12=Alonso-Floriano | first12=F. J.
| last13=Amado | first13=P. J. | last14=Bauer | first14=F. F.
| last15=Casal | first15=E. | last16=Diez Alonso | first16=E.
| last17=Herrero | first17=E. | last18=Morales | first18=J. C.
| last19=Mundt | first19=R. | last20=Ribas | first20=I.
| last21=Sarmiento | first21=L. F. | display-authors=1
| journal=Astronomy & Astrophysics
| volume=614 | id=A76 | pages=19 | date=June 2018
| arxiv=1802.02102 | bibcode=2018A&A...614A..76J
| doi=10.1051/0004-6361/201629599 | s2cid=56147445 }}</ref>

<ref name=Vedantham2020>{{Cite journal
| last1=Vedantham | first1=H. K. | last2=Callingham | first2=J. R.
| last3=Shimwell | first3=T. W. | last4=Tasse | first4=C.
| last5=Pope | first5=B. J. S. | last6=Bedell | first6=M.
| last7=Snellen | first7=I. | last8=Best | first8=P.
| last9=Hardcastle | first9=M. J. | last10=Haverkorn | first10=M.
| last11=Mechev | first11=A. | display-authors=1
| title=Coherent radio emission from a quiescent red dwarf indicative of star–planet interaction
| url=https://www.nature.com/articles/s41550-020-1011-9
| journal=] | bibcode=2020NatAs...4..577V
| language=en | pages=577–583 | date=2020-02-17
| volume=4 | issue=6 | doi=10.1038/s41550-020-1011-9 | issn=2397-3366 | arxiv=2002.08727 | hdl=1887/3133600 | s2cid=211204712 }}</ref>

<ref name="APJ-20200217">{{cite journal
| display-authors=1 | first1=Benjamin J. S. | last1=Pope
| first2=Megan | last2=Bedel | first3=Joseph R. | last3=Callingham
| first4=Harish K. | last4=Vedantham | first5=Ignas A. G. | last5=Snellen
| first6=Adrian M. | last6=Price-Whelan | first7=Timothy W. | last7=Shimwell
| title=No Massive Companion to the Coherent Radio-emitting M Dwarf GJ 1151
| journal=]
| volume=890 | number=2 | date=17 February 2020
| pages=L19 | bibcode=2020ApJ...890L..19P | arxiv=2002.07850
| doi=10.3847/2041-8213/ab5b99 | s2cid=211171765 | doi-access=free }}</ref>

<ref name="SA-20200229">{{cite news
| last=Starr | first=Michelle
| title=For The First Time, Astronomers Have Detected an Exoplanet Using Radio Waves
| url=https://www.sciencealert.com/a-new-way-to-search-for-exoplanets-has-yielded-a-distant-earth-sized-world
| date=29 February 2020 | work=ScienceAlert.com
| access-date=1 March 2020 }}</ref>

<ref name=SciNews>{{Cite web
| url=https://www.upi.com/Science_News/2020/02/18/Radio-telescope-measures-aurorae-in-distant-planetary-system/3421582042945/
| title=Radio telescope measures aurorae in distant planetary system
| website=UPI | language=en | access-date=2020-02-26 }}</ref>

<ref name=Redd2020>{{Cite web
| url=https://www.quantamagazine.org/new-exoplanet-search-strategy-claims-first-discovery-20200218/
| title=New Exoplanet Search Strategy Claims First Discovery
| last=Redd | first=Nola Taylor
| website=Quanta Magazine| date=18 February 2020
|language=en
| access-date=2020-02-26}}</ref>

<ref name=Clark>{{Cite web
| url=https://www.newscientist.com/article/2233972-an-exoplanet-is-generating-radio-waves-from-its-red-dwarf-sun/
| title=An exoplanet is generating radio waves from its red dwarf sun
| last=Clark|first=Stuart
| website=New Scientist | language=en-US
| access-date=2020-02-26 }}</ref>

<ref name=Mahadevan2021>{{citation|arxiv=2102.02233|year=2021|title=The Habitable-zone Planet Finder Detects a Terrestrial-mass Planet Candidate Closely Orbiting Gliese 1151: The Likely Source of Coherent Low-frequency Radio Emission from an Inactive Star|doi=10.3847/2041-8213/abe2b2|last1=Mahadevan|first1=Suvrath|author1-link=Suvrath Mahadevan|last2=Stefánsson|first2=Gudmundur|last3=Robertson|first3=Paul|last4=Terrien|first4=Ryan C.|last5=Ninan|first5=Joe P.|last6=Holcomb|first6=Rae J.|last7=Halverson|first7=Samuel|last8=Cochran|first8=William D.|last9=Kanodia|first9=Shubham|last10=Ramsey|first10=Lawrence W.|last11=Wolszczan|first11=Alexander|last12=Endl|first12=Michael|last13=Bender|first13=Chad F.|last14=Diddams|first14=Scott A.|last15=Fredrick|first15=Connor|last16=Hearty|first16=Fred|last17=Monson|first17=Andrew|last18=Metcalf|first18=Andrew J.|last19=Roy|first19=Arpita|last20=Schwab|first20=Christian|journal=The Astrophysical Journal Letters|volume=919|issue=1|pages=L9|bibcode=2021ApJ...919L...9M|s2cid=231802021 |doi-access=free }}</ref>

<ref name=Perger2021>{{citation|arxiv=2103.10216|year=2021|title=The CARMENES search for exoplanets around M dwarfs|doi=10.1051/0004-6361/202140786|last1=Perger|first1=M.|last2=Ribas|first2=I.|last3=Anglada-Escudé|first3=G.|last4=Morales|first4=J. C.|last5=Amado|first5=P. J.|last6=Caballero|first6=J. A.|last7=Quirrenbach|first7=A.|last8=Reiners|first8=A.|last9=Béjar|first9=V. J. S.|last10=Dreizler|first10=S.|last11=Galadí-Enríquez|first11=D.|last12=Hatzes|first12=A. P.|last13=Henning|first13=Th.|last14=Jeffers|first14=S. V.|last15=Kaminski|first15=A.|last16=Kürster|first16=M.|last17=Lafarga|first17=M.|last18=Montes|first18=D.|last19=Pallé|first19=E.|last20=Rodríguez-López|first20=C.|last21=Schweitzer|first21=A.|last22=Zapatero Osorio|first22=M. R.|last23=Zechmeister|first23=M.|journal=Astronomy & Astrophysics|volume=649|pages=L12|s2cid=126038821 |bibcode=2021A&A...649L..12P}}</ref>

<ref name="Blanco-Pozo2023">{{cite journal |last1=Blanco-Pozo |first1=J. |last2=Perger |first2=M. |display-authors=etal |date=March 2023 |title=The CARMENES search for exoplanets around M dwarfs. A long-period planet around GJ 1151 measured with CARMENES and HARPS-N data |journal=] |volume=671 |issue= |pages=A50 |doi=10.1051/0004-6361/202245053 |arxiv=2301.04442 |bibcode=2023A&A...671A..50B}}</ref>

}} }}


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{{Stars of Ursa Major}} {{Stars of Ursa Major}}


]
] ]
]
]
] ]
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{{stub}}

Latest revision as of 10:31, 1 December 2023

Red dwarf star
GJ 1151

Artist's impression of GJ 1151 and an orbiting planet
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Ursa Major
Right ascension 11 50 57.72053
Declination +48° 22′ 38.5612″
Apparent magnitude (V) 14.008
Characteristics
Spectral type dM4.5
B−V color index 1.787
Astrometry
Radial velocity (Rv)−36.13±0.26 km/s
Proper motion (μ) RA: -1545.069 mas/yr
Dec.: -962.724 mas/yr
Parallax (π)124.3378 ± 0.0549 mas
Distance26.23 ± 0.01 ly
(8.043 ± 0.004 pc)
Absolute magnitude (MV)14.482±0.022
Details
Mass0.1639±0.0093 M☉
Radius0.1781±0.0042 R☉
Luminosity (bolometric)0.003315±0.000018 L☉
Surface gravity (log g)5.09±0.09 cgs
Temperature3,143±26 K
Metallicity −0.12±0.10 dex
Rotation140±10 d
Rotational velocity (v sin i)2.0 km/s
Age2.5 Gyr
Other designations
GJ 1151, G 122-49, LHS 316, NLTT 28752, 2MASS J11505787+4822395, Gaia EDR3 786834302080370304
Database references
SIMBADdata

GJ 1151 is a star located in the northern circumpolar constellation of Ursa Major at a distance of 26.2 light-years (8.0 parsecs) from the Sun. It has a reddish hue and is too faint to be visible to the naked eye with an apparent visual magnitude of 14.0 The star is moving closer with a radial velocity of −36 km/s, and has a relatively large proper motion, traversing the celestial sphere at a rate of 1.815″·yr.

This is a small red dwarf star of spectral type dM4.5. It is 2.5 billion years old and is spinning with a projected rotational velocity of 2.0 km/s. The star has 15.4% of the mass of the Sun and 19.0% of the Sun's radius, with an effective temperature of 3,143 K.

Planetary system

In 2020, astronomers announced the discovery of radio emissions from the star which are consistent with the star having a magnetic interaction with a planet approximately the size of Earth, revolving in a 1-5 day long orbit. Such an interaction would be analogous to a scaled-up version of the Jupiter-Io magnetic interaction, with GJ 1151 taking the role of Jupiter and its planet the role of Io.

Two papers published only a month apart in 2021 discussed planet detection at GJ 1151 by the radial velocity method. One claimed the detection of a planet with a minimum mass of 2.5 ME and a period of 2 days, supporting the radio emission detection, while the other was unable to confirm this candidate planet, finding that the 2-day signal is likely caused by long-term variability, possibly connected to a more distant planet. This second study placed an upper limit of 0.7-1.2 ME on the minimum masses of any undetected planets with periods from 1-5 days.

In 2023, a different planet was found, with a minimum mass of 10.6 ME and a 390-day orbit, along with additional radial velocity variations. This new planet was referred to by the preprint version of the discovery paper as GJ 1151 b, but the published version of the paper, as well as the NASA Exoplanet Archive, refer to it as GJ 1151 c to differentiate it from the previous candidate. While the presence of a short-period planet associated with the radio emissions could not be completely ruled out, if such a planet exists its minimum mass must be less than 1.2 ME.

The GJ 1151 planetary system
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
c ≥10.62+1.31
−1.47 M🜨 		0.5714+0.0053
−0.0064 		389.7+5.4
−6.5 		— — —

See also

References

  1. ^ 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.
  2. ^ Houdebine, Éric R.; et al. (August 2019). "The Mass-Activity Relationships in M and K Dwarfs. I. Stellar Parameters of Our Sample of M and K Dwarfs". The Astronomical Journal. 158 (2): 17. arXiv:1905.07921. Bibcode:2019AJ....158...56H. doi:10.3847/1538-3881/ab23fe. S2CID 159041104. 56.
  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. ^ Blanco-Pozo, J.; Perger, M.; et al. (March 2023). "The CARMENES search for exoplanets around M dwarfs. A long-period planet around GJ 1151 measured with CARMENES and HARPS-N data". Astronomy & Astrophysics. 671: A50. arXiv:2301.04442. Bibcode:2023A&A...671A..50B. doi:10.1051/0004-6361/202245053.
  5. ^ Jeffers, S. V.; et al. (June 2018). "CARMENES input catalogue of M dwarfs. III. Rotation and activity from high-resolution spectroscopic observations". Astronomy & Astrophysics. 614: 19. arXiv:1802.02102. Bibcode:2018A&A...614A..76J. doi:10.1051/0004-6361/201629599. S2CID 56147445. A76.
  6. "G 122-49". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-03-02.
  7. Lépine, Sébastien; Shara, Michael M. (March 2005). "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)". The Astronomical Journal. 129 (3): 1483–1522. arXiv:astro-ph/0412070. Bibcode:2005AJ....129.1483L. doi:10.1086/427854. S2CID 2603568.
  8. Vedantham, H. K.; et al. (2020-02-17). "Coherent radio emission from a quiescent red dwarf indicative of star–planet interaction". Nature Astronomy. 4 (6): 577–583. arXiv:2002.08727. Bibcode:2020NatAs...4..577V. doi:10.1038/s41550-020-1011-9. hdl:1887/3133600. ISSN 2397-3366. S2CID 211204712.
  9. Pope, Benjamin J. S.; et al. (17 February 2020). "No Massive Companion to the Coherent Radio-emitting M Dwarf GJ 1151". The Astrophysical Journal Letters. 890 (2): L19. arXiv:2002.07850. Bibcode:2020ApJ...890L..19P. doi:10.3847/2041-8213/ab5b99. S2CID 211171765.
  10. Starr, Michelle (29 February 2020). "For The First Time, Astronomers Have Detected an Exoplanet Using Radio Waves". ScienceAlert.com. Retrieved 1 March 2020.
  11. "Radio telescope measures aurorae in distant planetary system". UPI. Retrieved 2020-02-26.
  12. Redd, Nola Taylor (18 February 2020). "New Exoplanet Search Strategy Claims First Discovery". Quanta Magazine. Retrieved 2020-02-26.
  13. Clark, Stuart. "An exoplanet is generating radio waves from its red dwarf sun". New Scientist. Retrieved 2020-02-26.
  14. Mahadevan, Suvrath; Stefánsson, Gudmundur; Robertson, Paul; Terrien, Ryan C.; Ninan, Joe P.; Holcomb, Rae J.; Halverson, Samuel; Cochran, William D.; Kanodia, Shubham; Ramsey, Lawrence W.; Wolszczan, Alexander; Endl, Michael; Bender, Chad F.; Diddams, Scott A.; Fredrick, Connor; Hearty, Fred; Monson, Andrew; Metcalf, Andrew J.; Roy, Arpita; Schwab, Christian (2021), "The Habitable-zone Planet Finder Detects a Terrestrial-mass Planet Candidate Closely Orbiting Gliese 1151: The Likely Source of Coherent Low-frequency Radio Emission from an Inactive Star", The Astrophysical Journal Letters, 919 (1): L9, arXiv:2102.02233, Bibcode:2021ApJ...919L...9M, doi:10.3847/2041-8213/abe2b2, S2CID 231802021
  15. ^ Perger, M.; Ribas, I.; Anglada-Escudé, G.; Morales, J. C.; Amado, P. J.; Caballero, J. A.; Quirrenbach, A.; Reiners, A.; Béjar, V. J. S.; Dreizler, S.; Galadí-Enríquez, D.; Hatzes, A. P.; Henning, Th.; Jeffers, S. V.; Kaminski, A.; Kürster, M.; Lafarga, M.; Montes, D.; Pallé, E.; Rodríguez-López, C.; Schweitzer, A.; Zapatero Osorio, M. R.; Zechmeister, M. (2021), "The CARMENES search for exoplanets around M dwarfs", Astronomy & Astrophysics, 649: L12, arXiv:2103.10216, Bibcode:2021A&A...649L..12P, doi:10.1051/0004-6361/202140786, S2CID 126038821
Known celestial objects within 20 light-years
Primary member type
Celestial objects by systems. Secondary members are listed in small print.
    0–10 ly →
Main-sequence
stars
A-type
G-type
M-type
(red dwarfs)
Brown dwarfs
L-type
  • Luhman 16 (6.5029±0.0011 ly)
  • T-type brown dwarf B
Sub-brown dwarfs
and rogue planets
Y-type
← 10–15 ly →
Subgiant stars
F-type
Main-sequence
stars
G-type
  • Tau Ceti (11.9118±0.0074 ly)
  • 4 (8?) planets: (b), (c), (d), e, f, g, h, (i)
K-type
M-type
(red dwarfs)
Degenerate
stars
White dwarfs
Brown dwarfs
T-type
← 15–20 ly    
Subgiant stars
G-type
Main-sequence
stars
A-type
G-type
K-type
M-type
(red dwarfs)
Degenerate
stars
White dwarfs
Brown dwarfs
L-type
T-type
Y-type
Sub-brown dwarfs
and rogue planets
Y-type
Italic are systems without known trigonometric parallax.
Constellation of Ursa Major
Stars
Bayer
Flamsteed
Variable
HR
HD
Other
Exoplanets
Nebulae
Galaxies
Messier
NGC
Other
Astronomical events
Category
Categories: