Gliese 832: Difference between revisions

Browse history interactively ← Previous editContent deleted Content addedVisual WikitextInline

Revision as of 17:24, 23 March 2023 editSevenSpheres (talk \| contribs)Extended confirmed users6,598 edits astrometric detection of planet← Previous edit		Latest revision as of 04:25, 19 December 2024 edit undoCitation bot (talk \| contribs)Bots5,409,604 edits Altered template type. Add: bibcode, doi, pages, volume, date, journal, title, arxiv, authors 1-19. Removed URL that duplicated identifier. Changed bare reference to CS1/2. \| Use this bot. Report bugs. \| Suggested by Jay8g \| #UCB_toolbar
(13 intermediate revisions by 9 users not shown)
Line 51:		Line 51:
	}}		}}
	{{Starbox catalog		{{Starbox catalog
	\| names = CD-49°13515, ] 204961, ] 106440, LHS 3685, PLX 5190<ref name="Simbad"/>		\| names = {{odlist \| 2MASS = J21333397-4900323 \| CD = -49°13515 \| GJ = 832 \| HD = 204961 \| HIP = 106440 \| L = 354-89 \| LHS = 3685 \| PLX = 5190 \| TIC = 139754153 \| TYC = 8431-60-1}}<ref name="Simbad"/>
	}}		}}
	{{Starbox reference		{{Starbox reference
Line 71:		Line 71:
	This star achieved ] some 52,920 years ago when it came within an estimated {{Convert\|4.817\|pc\|ly\|abbr=on\|lk=off\|order=flip}} of the Sun.<ref name=aa575_A35/>		This star achieved ] some 52,920 years ago when it came within an estimated {{Convert\|4.817\|pc\|ly\|abbr=on\|lk=off\|order=flip}} of the Sun.<ref name=aa575_A35/>

	Gliese 832 emits X-rays.<ref name=Schmitt/> Despite the strong ], Gliese 832 is producing on average less ionizing radiation than the Sun. Only at extremely short radiation wavelengths (<50nm) does its radiation intensity rise above the level of quiet Sun, but does not reach levels typical for active Sun.<ref>{{cite journal \|year=2016\|last1=Fontenla\|first1=J. M.\|last2=Linsky\|first2=Jeffrey L.\|last3=Garrison\|first3=Jesse\|last4=France\|first4=Kevin\|last5=Buccino\|first5=A.\|last6=Mauas\|first6=Pablo\|last7=Vietes\|first7=Mariela\|last8=Walkowicz\|first8=Lucianne M. \|title=Semi-Empirical Modeling of the Photosphere, Chromopshere, Transition Region, and Corona of the M-Dwarf Host Star Gj 832 \|journal=The Astrophysical Journal \|volume=830 \|issue=2 \|doi=10.3847/0004-637X/830/2/154 \|bibcode=2016ApJ...830..154F \|pages=154\|hdl=11336/21732\|s2cid=119279568 \|hdl-access=free}}</ref>		Gliese 832 emits X-rays.<ref name=Schmitt/> Despite the strong ], Gliese 832 is producing on average less ionizing radiation than the Sun. Only at extremely short radiation wavelengths (<50nm) does its radiation intensity rise above the level of quiet Sun, but does not reach levels typical for active Sun.<ref>{{cite journal \|year=2016\|last1=Fontenla\|first1=J. M.\|last2=Linsky\|first2=Jeffrey L.\|last3=Garrison\|first3=Jesse\|last4=France\|first4=Kevin\|last5=Buccino\|first5=A.\|last6=Mauas\|first6=Pablo\|last7=Vietes\|first7=Mariela\|last8=Walkowicz\|first8=Lucianne M. \|title=Semi-Empirical Modeling of the Photosphere, Chromopshere, Transition Region, and Corona of the M-Dwarf Host Star Gj 832 \|journal=The Astrophysical Journal \|volume=830 \|issue=2 \|doi=10.3847/0004-637X/830/2/154 \|bibcode=2016ApJ...830..154F \|pages=154\|hdl=11336/21732\|s2cid=119279568 \|hdl-access=free \|doi-access=free \|arxiv=1608.00934 }}</ref>

	==Planetary system==		==Planetary system==
			Gliese 832 hosts one known planet, with a second planet having been refuted in 2022.<ref name=Gorrini2022/> No additional planets were found as of 2024.<ref>{{cite journal \| arxiv=2409.01173 \| last1=Liebing \| first1=F. \| last2=Jeffers \| first2=S. V. \| last3=Gorrini \| first3=P. \| last4=Haswell \| first4=C. A. \| last5=Dreizler \| first5=S. \| last6=Barnes \| first6=J. R. \| last7=Hartogh \| first7=C. \| last8=Koseleva \| first8=V. \| last9=Del Sordo \| first9=F. \| last10=Amado \| first10=P. J. \| last11=Caballero \| first11=J. A. \| last12=López-González \| first12=M. J. \| last13=Morales \| first13=N. \| last14=Reiners \| first14=A. \| last15=Ribas \| first15=I. \| last16=Quirrenbach \| first16=A. \| last17=Rodríguez \| first17=E. \| last18=Tal-Or \| first18=L. \| last19=Tsapras \| first19=Y. \| title=RedDots: Limits on habitable and undetected planets orbiting nearby stars GJ 832, GJ 674, and Ross 128 \| journal=Astronomy and Astrophysics \| date=2024 \| volume=690 \| pages=A234 \| doi=10.1051/0004-6361/202347902 \| bibcode=2024A&A...690A.234L }}</ref>
	Gliese 832 hosts one known planet, with a second planet having been refuted in 2022.<ref name=Gorrini2022/>
	{{OrbitboxPlanet begin		{{OrbitboxPlanet begin
	\| table_ref = <ref name="Xiao2023"/>		\| table_ref = <ref name="Xiao2023"/>
Line 94:		Line 94:

	===Gliese 832 c===		===Gliese 832 c===
		⚫	Gliese 832 c was believed to be of ] mass.{{r\|Mike Wall}} It was announced to orbit in the optimistic ] but outside the conservative habitable zone of its parent star.<ref name="Wittenmyer14" /> The planet Gliese 832 c was believed to be in, or very close to, the right distance from its sun to allow liquid water to exist on its surface.{{r\|Mike Wall}} However, doubts were raised about the existence of planet c by a 2015 study, which found that its orbital period is close to the stellar rotation period.<ref name=mnras452_3_2745/> The existence of the planet was refuted in 2022, when a study found that the ] signal shows characteristics of a signal originating from stellar activity, and not from a planet.<ref name=Gorrini2022/>
	{{Main\|Gliese 832 c}}
⚫	~~In 2014, a second planet, ], was discovered by astronomers at the University of New South Wales. This planet~~ was believed to be of ] mass.{{r\|Mike Wall}} It was announced to orbit in the optimistic ] but outside the conservative habitable zone of its parent star.<ref name="Wittenmyer14" /> The planet Gliese 832 c was believed to be in, or very close to, the right distance from its sun to allow liquid water to exist on its surface.{{r\|Mike Wall}} However, doubts were raised about the existence of planet c by a 2015 study, which found that its orbital period is close to the stellar rotation period.<ref name=mnras452_3_2745/> The existence of the planet was refuted in 2022, when a study found that the ] signal shows characteristics of a signal originating from stellar activity, and not from a planet.<ref name=Gorrini2022/>

	The region between Gliese 832 b and Gliese 832 c is a zone where additional planets are possible.<ref>{{citation\|arxiv=1604.04544\|title=Dynamics of a Probable Earth-mass Planet in GJ 832 System\|year=2016\|doi=10.3847/1538-4357/aa80e2\|last1=Satyal\|first1=S.\|last2=Griffith\|first2=J.\|last3=Musielak\|first3=Z. E.\|journal=The Astrophysical Journal\|volume=845\|issue=2\|page=106\|s2cid=118663957}}</ref>		The region between Gliese 832 b and where Gliese 832 c would be is a zone where additional planets are possible.<ref>{{citation\|arxiv=1604.04544\|title=Dynamics of a Probable Earth-mass Planet in GJ 832 System\|year=2016\|doi=10.3847/1538-4357/aa80e2\|last1=Satyal\|first1=S.\|last2=Griffith\|first2=J.\|last3=Musielak\|first3=Z. E.\|journal=The Astrophysical Journal\|volume=845\|issue=2\|page=106\|s2cid=118663957 \|doi-access=free }}</ref>

	===Search for cometary disc===		===Search for cometary disc===
Line 125:		Line 124:
	\| volume=918 \| issue=1 \| id=40 \| pages=23 \| date=September 2021		\| volume=918 \| issue=1 \| id=40 \| pages=23 \| date=September 2021
	\| doi=10.3847/1538-4357/ac0aea \| arxiv=2106.07656		\| doi=10.3847/1538-4357/ac0aea \| arxiv=2106.07656
	\| bibcode=2021ApJ...918...40P \| s2cid=235435757}}</ref>		\| bibcode=2021ApJ...918...40P \| s2cid=235435757 \| doi-access=free }}</ref>

	<ref name=nodebris>		<ref name=nodebris>
Line 251:		Line 250:
	\|bibcode=1995ApJ...450..392S		\|bibcode=1995ApJ...450..392S
	\|doi=10.1086/176149		\|doi=10.1086/176149
			\|doi-access=free
	}}</ref>		}}</ref>

	<ref name="Mike Wall">"Nearby Alien Planet May Be Capable of Supporting Life", Mike Wall, Space.com, June 25, 2014, http://www.space.com/26357-exoplanet-habitable-zone-gliese-832c.html</ref>		<ref name="Mike Wall">"Nearby Alien Planet May Be Capable of Supporting Life", Mike Wall, Space.com, June 25, 2014, http://www.space.com/26357-exoplanet-habitable-zone-gliese-832c.html {{Webarchive\|url=https://web.archive.org/web/20180712234753/http://www.space.com/26357-exoplanet-habitable-zone-gliese-832c.html \|date=2018-07-12 }}</ref>

	<ref name=aa575_A35>{{citation		<ref name=aa575_A35>{{citation
Line 265:		Line 265:
	}}</ref>		}}</ref>

	<ref name="Lindgren2017">{{cite journal \| title=Metallicity determination of M dwarfs. Expanded parameter range in metallicity and effective temperature \| url=https://www.aanda.org/articles/aa/full_html/2017/08/aa30715-17/aa30715-17.html \| last1=Lindgren \| first1=Sara \| last2=Heiter \| first2=Ulrike \| journal=Astronomy and Astrophysics \| volume=604 \| pages=A97 \| year=2017 \| arxiv=1705.08785 \| bibcode=2017A&A...604A..97L \| doi=10.1051/0004-6361/201730715 \| s2cid=119216828 }}</ref>		<ref name="Lindgren2017">{{cite journal \| title=Metallicity determination of M dwarfs. Expanded parameter range in metallicity and effective temperature \| url=https://www.aanda.org/articles/aa/full_html/2017/08/aa30715-17/aa30715-17.html \| last1=Lindgren \| first1=Sara \| last2=Heiter \| first2=Ulrike \| journal=Astronomy and Astrophysics \| volume=604 \| pages=A97 \| year=2017 \| arxiv=1705.08785 \| bibcode=2017A&A...604A..97L \| doi=10.1051/0004-6361/201730715 \| s2cid=119216828 \| access-date=2018-09-03 \| archive-date=2021-01-23 \| archive-url=https://web.archive.org/web/20210123180529/https://www.aanda.org/articles/aa/full_html/2017/08/aa30715-17/aa30715-17.html \| url-status=live }}</ref>

	<ref name="Simbad">{{cite simbad \| title=Gliese 832 \| access-date=2018-09-23 }}</ref>		<ref name="Simbad">{{cite simbad \| title=Gliese 832 \| access-date=2018-09-23 }}</ref>
Line 276:		Line 276:
	\| journal=Monthly Notices of the Royal Astronomical Society		\| journal=Monthly Notices of the Royal Astronomical Society
	\| volume=452 \| issue=3 \| pages=2745–2756 \| date=September 2015		\| volume=452 \| issue=3 \| pages=2745–2756 \| date=September 2015
	\| doi=10.1093/mnras/stv1441 \| bibcode=2015MNRAS.452.2745S		\| doi=10.1093/mnras/stv1441 \| doi-access=free \| bibcode=2015MNRAS.452.2745S
	\| arxiv=1506.08039 \| s2cid=119181646 \| postscript=.		\| arxiv=1506.08039 \| s2cid=119181646 \| postscript=.
	}}</ref>		}}</ref>
Line 284:		Line 284:
	<ref name=Gorrini2022>{{cite journal \|last1=Gorrini \|first1=P. \|last2=Astudillo-Defru \|first2=N. \|display-authors=etal \|date=August 2022 \|title=Detailed stellar activity analysis and modelling of GJ 832: Reassessment of the putative habitable zone planet GJ 832c \|journal=] \|volume=664 \|issue= \|pages=A64 \|doi=10.1051/0004-6361/202243063 \|arxiv=2206.07552 \|bibcode=2022A&A...664A..64G\|s2cid=249674385 }}</ref>		<ref name=Gorrini2022>{{cite journal \|last1=Gorrini \|first1=P. \|last2=Astudillo-Defru \|first2=N. \|display-authors=etal \|date=August 2022 \|title=Detailed stellar activity analysis and modelling of GJ 832: Reassessment of the putative habitable zone planet GJ 832c \|journal=] \|volume=664 \|issue= \|pages=A64 \|doi=10.1051/0004-6361/202243063 \|arxiv=2206.07552 \|bibcode=2022A&A...664A..64G\|s2cid=249674385 }}</ref>

	<ref name="Xiao2023">{{cite journal \|last1=Xiao \|first1=Guang-Yao \|last2=Liu \|first2=Yu-Juan \|display-authors=etal \|date=March 2023 \|title=The Masses of a Sample of Radial-Velocity Exoplanets with Astrometric Measurements \|journal=] \|volume= \|issue= \|pages= \|doi= \|arxiv=2303.12409}}</ref>		<ref name="Xiao2023">{{cite journal \|last1=Xiao \|first1=Guang-Yao \|last2=Liu \|first2=Yu-Juan \|display-authors=etal \|date=March 2023 \|title=The Masses of a Sample of Radial-Velocity Exoplanets with Astrometric Measurements \|journal=] \|volume= 23\|issue= 5\|pages= \|doi= 10.1088/1674-4527/accb7e\|arxiv=2303.12409\|bibcode=2023RAA....23e5022X \|s2cid=257663647 }}</ref>

	}}		}}
Line 302:		Line 302:
	]		]
	]		]
	]		]
			]

Latest revision as of 04:25, 19 December 2024

Star in the constellation Grus

Gliese 832
Observation data Epoch J2000.0 Equinox J2000.0
Gliese 832Location of Gliese 832 in the constellation Grus
Constellation	Grus
Right ascension	21 33 33.97512
Declination	−49° 00′ 32.3994″
Apparent magnitude (V)	8.66
Characteristics
Evolutionary stage	main-sequence star
Spectral type	M2V
B−V color index	1.52
Astrometry

Radial velocity (R_v)	12.72±0.13 km/s
Proper motion (μ)	RA: −45.917 mas/yr Dec.: −816.875 mas/yr
Parallax (π)	201.3252 ± 0.0237 mas
Distance	16.200 ± 0.002 ly (4.9671 ± 0.0006 pc)
Absolute magnitude (M_V)	10.19

Details

Mass	0.441 ± 0.011 `M`_☉
Radius	0.442 ± 0.018 `R`_☉
Luminosity (bolometric)	0.0276 ± 0.0009 `L`_☉
Luminosity (visual, L_V)	0.007 `L`_☉
Surface gravity (log g)	4.7 cgs
Temperature	3,539+79 −74 K
Metallicity	−0.06 ± 0.04 dex
Rotation	37.5+1.4 −1.5 d
Age	6±1.5 Gyr

Other designations
CD−49°13515, GJ 832, HD 204961, HIP 106440, L 354-89, LHS 3685, PLX 5190, TIC 139754153, TYC 8431-60-1, 2MASS J21333397-4900323
Database references
SIMBAD	The star
	planet c
	planet b
Exoplanet Archive	data
Data sources:
Hipparcos Catalogue, HD

Gliese 832 (Gl 832 or GJ 832) is a red dwarf of spectral type M2V in the southern constellation Grus. The apparent visual magnitude of 8.66 means that it is too faint to be seen with the naked eye. It is located relatively close to the Sun, at a distance of 16.2 light years and has a high proper motion of 818.16 milliarcseconds per year. Gliese 832 has just under half the mass and radius of the Sun. Its estimated rotation period is a relatively leisurely 46 days. The star is roughly 6 billion years old.

This star achieved perihelion some 52,920 years ago when it came within an estimated 15.71 ly (4.817 pc) of the Sun.

Gliese 832 emits X-rays. Despite the strong flare activity, Gliese 832 is producing on average less ionizing radiation than the Sun. Only at extremely short radiation wavelengths (<50nm) does its radiation intensity rise above the level of quiet Sun, but does not reach levels typical for active Sun.

Planetary system

Gliese 832 hosts one known planet, with a second planet having been refuted in 2022. No additional planets were found as of 2024.

The Gliese 832 planetary system
Companion (in order from star)	Mass	Semimajor axis (AU)	Orbital period (years)	Eccentricity	Inclination	Radius
b	0.8+0.12 −0.11 M_J	3.53+0.15 −0.16	9.88+0.34 −0.33	0.069+0.026 −0.027	54.9+6.6 −4.9 or 125.1+4.9 −6.6°	—

Gliese 832 b

Main article: Gliese 832 b

In September 2008, it was announced that a Jupiter-like planet, designated Gliese 832 b, had been detected in a long-period, near-circular orbit around this star, with a false alarm probability of a negligible 0.05%. It would induce an astrometric perturbation on its star of at least 0.95 milliarcseconds and is thus a good candidate for being detected by astrometric observations. Despite its relatively large angular distance, direct imaging is problematic due to the star–planet contrast. The orbital solution of the planet was refined in 2011. In 2023, an astrometric detection of the planet was announced, determining its inclination and revealing a true mass 80% the mass of Jupiter.

Gliese 832 c

Gliese 832 c was believed to be of super-Earth mass. It was announced to orbit in the optimistic habitable zone but outside the conservative habitable zone of its parent star. The planet Gliese 832 c was believed to be in, or very close to, the right distance from its sun to allow liquid water to exist on its surface. However, doubts were raised about the existence of planet c by a 2015 study, which found that its orbital period is close to the stellar rotation period. The existence of the planet was refuted in 2022, when a study found that the radial velocity signal shows characteristics of a signal originating from stellar activity, and not from a planet.

The region between Gliese 832 b and where Gliese 832 c would be is a zone where additional planets are possible.

Search for cometary disc

If this system has a comet disc, it is not "brighter than the fractional dust luminosity 10" according to a 2012 Herschel study.

Notes

Using the absolute visual magnitude of Gliese 832 $\scriptstyle M_{V_{\ast }}=10.19$ and the absolute visual magnitude of the Sun $\scriptstyle M_{V_{\odot }}=4.83$ , the visual luminosity can be calculated by $\scriptstyle {\frac {L_{V_{\ast }}}{L_{V_{\odot }}}}=10^{0.4\left(M_{V_{\odot }}-M_{V_{\ast }}\right)}$

References

^ 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.
^ Bailey, J.; Butler, R. P.; Tinney, C. G.; Jones, H. R. A.; O'Toole, S.; Carter, B. D.; Marcy, G. W. (2009). "A Jupiter-like Planet Orbiting the Nearby M Dwarf GJ832". The Astrophysical Journal. 690 (1): 743–747. arXiv:0809.0172. Bibcode:2009ApJ...690..743B. doi:10.1088/0004-637X/690/1/743. S2CID 17172233.
^ Suárez Mascareño, A.; et al. (September 2015), "Rotation periods of late-type dwarf stars from time series high-resolution spectroscopy of chromospheric indicators", Monthly Notices of the Royal Astronomical Society, 452 (3): 2745–2756, arXiv:1506.08039, Bibcode:2015MNRAS.452.2745S, doi:10.1093/mnras/stv1441, S2CID 119181646.
^ 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.
Lindgren, Sara; Heiter, Ulrike (2017). "Metallicity determination of M dwarfs. Expanded parameter range in metallicity and effective temperature". Astronomy and Astrophysics. 604: A97. arXiv:1705.08785. Bibcode:2017A&A...604A..97L. doi:10.1051/0004-6361/201730715. S2CID 119216828. Archived from the original on 2021-01-23. Retrieved 2018-09-03.
^ Gorrini, P.; Astudillo-Defru, N.; et al. (August 2022). "Detailed stellar activity analysis and modelling of GJ 832: Reassessment of the putative habitable zone planet GJ 832c". Astronomy & Astrophysics. 664: A64. arXiv:2206.07552. Bibcode:2022A&A...664A..64G. doi:10.1051/0004-6361/202243063. S2CID 249674385.
"Gliese 832". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-09-23.
^ "Nearby Alien Planet May Be Capable of Supporting Life", Mike Wall, Space.com, June 25, 2014, http://www.space.com/26357-exoplanet-habitable-zone-gliese-832c.html Archived 2018-07-12 at the Wayback Machine
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.
Schmitt, J. H. M. M.; Fleming, T. A.; Giampapa, M. S. (1995). "The X-ray view of the low-mass stars in the solar neighborhood". The Astrophysical Journal. 450 (9): 392–400. Bibcode:1995ApJ...450..392S. doi:10.1086/176149.
Fontenla, J. M.; Linsky, Jeffrey L.; Garrison, Jesse; France, Kevin; Buccino, A.; Mauas, Pablo; Vietes, Mariela; Walkowicz, Lucianne M. (2016). "Semi-Empirical Modeling of the Photosphere, Chromopshere, Transition Region, and Corona of the M-Dwarf Host Star Gj 832". The Astrophysical Journal. 830 (2): 154. arXiv:1608.00934. Bibcode:2016ApJ...830..154F. doi:10.3847/0004-637X/830/2/154. hdl:11336/21732. S2CID 119279568.
Liebing, F.; Jeffers, S. V.; Gorrini, P.; Haswell, C. A.; Dreizler, S.; Barnes, J. R.; Hartogh, C.; Koseleva, V.; Del Sordo, F.; Amado, P. J.; Caballero, J. A.; López-González, M. J.; Morales, N.; Reiners, A.; Ribas, I.; Quirrenbach, A.; Rodríguez, E.; Tal-Or, L.; Tsapras, Y. (2024). "RedDots: Limits on habitable and undetected planets orbiting nearby stars GJ 832, GJ 674, and Ross 128". Astronomy and Astrophysics. 690: A234. arXiv:2409.01173. Bibcode:2024A&A...690A.234L. doi:10.1051/0004-6361/202347902.
^ Xiao, Guang-Yao; Liu, Yu-Juan; et al. (March 2023). "The Masses of a Sample of Radial-Velocity Exoplanets with Astrometric Measurements". Research in Astronomy and Astrophysics. 23 (5). arXiv:2303.12409. Bibcode:2023RAA....23e5022X. doi:10.1088/1674-4527/accb7e. S2CID 257663647.
Bonfils, Xavier; Delfosse, Xavier; Udry, Stéphane; Forveille, Thierry; Mayor, Michel; Perrier, Christian; Bouchy, François; Gillon, Michaël; Lovis, Christophe; Pepe, Francesco; Queloz, Didier; Santos, Nuno C.; Ségransan, Damien; Bertaux, Jean-Loup (2011). "The HARPS search for southern extra-solar planets XXXI. The M-dwarf sample". Astronomy and Astrophysics. 549: A109. arXiv:1111.5019. Bibcode:2013A&A...549A.109B. doi:10.1051/0004-6361/201014704. S2CID 119288366.
Wittenmyer, R.A.; Tuomi, M.; Butler, R.P.; Jones, H. R. A.; O'Anglada-Escude, G.; Horner, J.; Tinney, C.G.; Marshall, J.P.; Carter, B.D.; et al. (2014). "GJ 832c: A super-earth in the habitable zone". The Astrophysical Journal. 1406 (2): 5587. arXiv:1406.5587. Bibcode:2014ApJ...791..114W. doi:10.1088/0004-637X/791/2/114. S2CID 12157837.
Satyal, S.; Griffith, J.; Musielak, Z. E. (2016), "Dynamics of a Probable Earth-mass Planet in GJ 832 System", The Astrophysical Journal, 845 (2): 106, arXiv:1604.04544, doi:10.3847/1538-4357/aa80e2, S2CID 118663957
B. C. Matthews; forthcoming study promised in Lestrade, J.-F.; Matthews, B. C.; Sibthorpe, B.; Kennedy, G. M.; Wyatt, M. C.; Bryden, G.; Greaves, J. S.; Thilliez, E.; Moro-Martín, A.; Booth, M.; Dent, W. R. F.; Duchêne, G.; Harvey, P. M.; Horner, J.; Kalas, P.; Kavelaars, J. J.; Phillips, N. M.; Rodriguez, D. R.; Su, K. Y. L.; Wilner, D. J. (2012). "A DEBRIS Disk Around The Planet Hosting M-star GJ581 Spatially Resolved with Herschel". Astronomy and Astrophysics. 548: A86. arXiv:1211.4898. Bibcode:2012A&A...548A..86L. doi:10.1051/0004-6361/201220325. S2CID 53704989.

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	Sirius (Alpha Canis Majoris) (8.7094±0.0054 ly) white dwarf B
G-type	Sun (0 ly) rest of Solar System Alpha Centauri α Cen (Rigil Kentaurus) (4.3441±0.0022 ly) K-type main-sequence star B (Toliman) red dwarf C (Proxima Centauri) (4.2465 ± 0.0003 ly) 2 (5?) planets: Ab?; Bc?; Cb, Cc?, Cd
M-type (red dwarfs)	Barnard's Star (5.9629±0.0004 ly) Wolf 359 (7.8558±0.0013 ly) 1? planets: b? Lalande 21185 (8.3044±0.0007 ly) 2 (3?) planets: b, d?, c Gliese 65 A (BL Ceti) (8.724±0.012 ly) red dwarf B (UV Ceti) Ross 154 (9.7063±0.0009 ly)

Brown dwarfs

L-type	Luhman 16 (6.5029±0.0011 ly) T-type brown dwarf B

Sub-brown dwarfs
and rogue planets

Y-type	WISE 0855−0714 (7.430±0.041 ly)

← 10–15 ly →

Subgiant stars

F-type	Procyon (Alpha Canis Minoris) (11.402±0.032 ly) white dwarf B

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	Epsilon Eridani (Ran) (10.4749±0.0037 ly) 1 (2?) planets: b (Ægir), c? 61 Cygni (11.4039±0.0012 ly) K-type main-sequence star B Epsilon Indi (11.8670±0.0041 ly) 2 T-type brown dwarfs: Ba, Bb planet Ab
M-type (red dwarfs)	Ross 248 (10.3057±0.0014 ly) Lacaille 9352 (10.7241±0.0007 ly) 2 (3?) planets: b, c, d? Ross 128 (11.0074±0.0011 ly) planet b EZ Aquarii (11.109±0.034 ly) 2 red dwarfs: B, C Struve 2398 (11.4908±0.0009 ly) red dwarf B 2? planets: Bb?, Bc? Groombridge 34 (11.6191±0.0008 ly) red dwarf B 2 planets: Ab, Ac DX Cancri (11.6797±0.0027 ly) GJ 1061 (11.9839±0.0014 ly) 3 planets: b, c, d YZ Ceti (12.1222±0.0015 ly) 3 planets: b, c, d Luyten's Star (12.3485±0.0019 ly) 2 (4?) planets: b, c, d?, e? Teegarden's Star (12.4970±0.0045 ly) 2 planets: b, c Kapteyn's Star (12.8308±0.0008 ly) Lacaille 8760 (12.9472±0.0018 ly) SCR 1845−6357 (13.0638±0.0070 ly) T-type brown dwarf B Kruger 60 (13.0724±0.0052 ly) red dwarf B DENIS J1048−3956 (13.1932±0.0027 ly) Ross 614 (13.363±0.040 ly) red dwarf B Wolf 1061 (14.0500±0.0016 ly) 3 planets: b, c, d Gliese 1 (14.1747±0.0022 ly) TZ Arietis (14.5780±0.0046 ly) planet b Wolf 424 (14.595±0.031 ly) red dwarf B Gliese 687 (14.8395±0.0014 ly) 2 planets: b, c Gliese 674 (14.8492±0.0018 ly) planet b LHS 292 (14.8706±0.0041 ly)

Degenerate
stars

White dwarfs	van Maanen 2 (14.0718±0.0011 ly)

Brown dwarfs

T-type	UGPS J0722-0540 (13.43±0.13 ly)

← 15–20 ly

Subgiant stars

G-type	Delta Pavonis (19.893±0.015 ly)

Main-sequence
stars

A-type	Altair (Alpha Aquilae) (16.730±0.049 ly)
G-type	Alsafi (Sigma Draconis) (18.7993±0.0081 ly) Achird (Eta Cassiopeiae) (19.3314±0.0025 ly) K-type main-sequence star B e (82 G.) Eridani (19.7045±0.0093 ly) 3 (6?) planets: b, c?, d (c), e?, f?, g?, d
K-type	Groombridge 1618 (15.8857±0.0017 ly) Omicron (40) Eridani (16.3330±0.0042 ly) white dwarf B red dwarf C 70 Ophiuchi (16.7074±0.0087 ly) K-type main-sequence star B Gliese 570 (19.1987±0.0074 ly) 2 red dwarfs: B, C T-type brown dwarf D 36 Ophiuchi (19.4185±0.0036 ly) 2 K-type main-sequence stars: B, C HR 7703 (19.609±0.013 ly) red dwarf B
M-type (red dwarfs)	GJ 1245 (15.2001±0.0034 ly) 2 red dwarfs: B, C Gliese 876 (15.2382±0.0025 ly) 4 planets: d, c, b, e LHS 288 (15.7586±0.0034 ly) GJ 1002 (15.8060±0.0036 ly) 2 planets: b, c Gliese 412 (15.9969±0.0026 ly) red dwarf B AD Leonis (16.1939±0.0024 ly) Gliese 832 (16.2005±0.0019 ly) planet b Gliese 682 (16.3328±0.0026 ly) 2? planets: b?, c? EV Lacertae (16.4761±0.0018 ly) G 9-38 (16.800±0.011 ly) red dwarf B GJ 3379 (16.9861±0.0027 ly) Gliese 445 (17.1368±0.0017 ly) 2M1540 (17.3738±0.0046 ly) GJ 3323 (17.5309±0.0026 ly) 2 planets: b, c Gliese 526 (17.7263±0.0024 ly) Stein 2051 (17.9925±0.0020 ly) white dwarf B Gliese 251 (18.2146±0.0028 ly) planet b LP 816-60 (18.3305±0.0038 ly) LSR J1835+3259 (18.5534±0.0049 ly) Gliese 205 (18.6042±0.0022 ly) Gliese 229 (18.7906±0.0018 ly) T-type brown dwarf B 2 planets: Ab, Ac Ross 47 (18.8883±0.0031 ly) Gliese 693 (19.2078±0.0053 ly) Gliese 754 (19.2724±0.0067 ly) Gliese 908 (19.2745±0.0032 ly) Gliese 752 (19.2922±0.0027 ly) red dwarf B (vB 10) planet Ab Gliese 588 (19.2996±0.0031 ly) 2? planets: b?, c? YZ Canis Minoris (19.5330±0.0040 ly) GJ 1005 (19.577±0.035 ly) red dwarf B Gliese 268 (19.7414±0.0076 ly) red dwarf B

Degenerate
stars

White dwarfs	Gliese 440 (15.1226±0.0013 ly)

Brown dwarfs

L-type	DENIS 0255−4700 (15.877±0.014 ly)
T-type	WISE 1741+2553 (15.22±0.20 ly) WISE 1506+7027 (16.856±0.052 ly) DENIS 0817-6155 (17.002±0.037 ly) 2MASS 0939-2448 (17.41±0.44 ly) T-type brown dwarf B 2MASS 1114-2618 (18.20±0.14 ly) 2MASS 0415-0935 (18.62±0.18 ly) SIMP0136 (19.955±0.057 ly) 2MASS 0937+2931 (19.96 _−0.21 ly)
Y-type	WISE 1639−6847 (15.450±0.041 ly) WISE 0350−5658 (18.49±0.24 ly)

Sub-brown dwarfs
and rogue planets

Y-type	WISE 1541−2250 (19.54±0.24 ly)

Italic are systems without known trigonometric parallax.

Constellation of Grus

Stars

Bayer	α (Alnair) β (Tiaki) γ (Aldhanab) δ δ ε ζ η θ ι κ λ μ μ ν ξ ο π π ρ σ σ τ τ τ υ φ
Variable	RZ CE
HR	8323 8501
HD	208487 (Itonda) 213240 215456
Other	2MASS J22282889–4310262 Gliese 832 PSR J2144−3933 S5-HVS1 WASP-95 WISE 2220−3628

Exoplanets	Gliese 832 b HD 208487 b HD 213240 b τ Gruis b

Galaxies

NGC	7070 7070A 7072 7075 7079 7087 7213 7418 7424 7496 7531 7552 7582 7590
Other	IC 1459 IC 5201

Galaxy clusters	Abell S1063

Misplaced Pages