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Revision as of 01:18, 3 November 2020 editTrurle (talk | contribs)Autopatrolled, Extended confirmed users, Pending changes reviewers16,588 edits →Planetary system: moving orbitbox to proper section and referencing← Previous edit Revision as of 01:27, 3 November 2020 edit undoTrurle (talk | contribs)Autopatrolled, Extended confirmed users, Pending changes reviewers16,588 edits →Planetary system: more data on planet bNext edit →
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Gliese 832 hosts two known planets. Gliese 832 hosts two known planets.
{{OrbitboxPlanet begin {{OrbitboxPlanet begin
|table_ref=<ref name=Bonfils2011>{{citation|arxiv=1111.5019|title=The HARPS search for southern extra-solar planets XXXI. The M-dwarf sample|year=2011}}
|table_ref=
}} }}
{{OrbitboxPlanet {{OrbitboxPlanet
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{{OrbitboxPlanet {{OrbitboxPlanet
| exoplanet = ] | exoplanet = ]
| mass = ≥0.64 ± 0.06 | mass = ≥0.62
| period = 3416 ± 131 | period = 3507{{±|181}}
| semimajor = 3.4 ± 0.4 | semimajor = 3.46
| eccentricity = 0.12 ± 0.11 | eccentricity = 0.08{{±|0.05}}
}} }}
{{Orbitbox end}} {{Orbitbox end}}
⚫ In September 2008, it was announced that a ]-like planet, now designated as ], had been detected in a long-period, near-circular orbit around this star (false alarm probability thus far: a negligible 0.05%). It would induce an ] perturbation on its star of at least 0.95 ]s 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.<ref name="bailey08" /> The orbital solution of the planet was refined in 2011.<ref name=Bonfils2011/>
===Discovery of Jupiter mass planet===
⚫ In September 2008, it was announced that a ]-like planet, now designated as ], had been detected in a long-period, near-circular orbit around this star (false alarm probability thus far: a negligible 0.05%). It would induce an ] perturbation on its star of at least 0.95 ]s 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.<ref name="bailey08" />


⚫ In 2014, a second planet ] was discovered by astronomers at the University of New South Wales. This one is believed to be of super-Earth mass{{r|Mike Wall}} and has since been given the scientific name ].{{r|Mike Wall}} It was announced to orbit in the optimistic ] but outside the conservative habitable zone of its parent star.<ref name="Wittenmyer14" />
===Discovery of Gliese 832 c (super-Earth mass planet) in habitable zone===
⚫ In 2014, a second planet was discovered by astronomers at the University of New South Wales. This one is believed to be of super-Earth mass{{r|Mike Wall}} and has since been given the scientific name ].{{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 is 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}} The planet is 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}}

Revision as of 01:27, 3 November 2020

Gliese 832
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Grus
Right ascension 21 33 33.9750
Declination −49° 00′ 32.4035″
Apparent magnitude (V) 8.66
Characteristics
Spectral type M2V
B−V color index 1.52
Astrometry
Radial velocity (Rv)18.0 km/s
Proper motion (μ) RA: −45.834±0.071 mas/yr
Dec.: −816.604±0.064 mas/yr
Parallax (π)201.4073 ± 0.0429 mas
Distance16.194 ± 0.003 ly
(4.965 ± 0.001 pc)
Absolute magnitude (MV)10.19
Details
Mass0.45 ± 0.05 M☉
Radius0.48 R☉
Luminosity (bolometric)0.035 L☉
Luminosity (visual, LV)0.007 L☉
Surface gravity (log g)4.7 cgs
Temperature3,620 K
Metallicity −0.06±0.04 dex
Rotation45.7±9.3 d
Age9.24 Gyr
Other designations
CD-49°13515, HD 204961, HIP 106440, LHS 3685, PLX 5190
Database references
SIMBADThe star
planet c
planet b
Exoplanet Archivedata
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 818.93 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 9.5 billion years old.

In 2014, Gliese 832 was announced to be hosting the closest potentially habitable Earth-mass-range exoplanet to the Solar System. This star achieved perihelion some 52,920 years ago when it came within an estimated 15.71 ly (4.817 pc) of the Sun.

Planetary system

Gliese 832 hosts two known planets.

The Gliese 832 planetary systemCite error: A <ref> tag is missing the closing </ref> (see the help page).
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius


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 Grus
Stars
Bayer
Variable
HR
HD
Other
Exoplanets
Galaxies
NGC
Other
Galaxy clusters
Category
  1. ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. ^ 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.
  3. ^ 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.{{citation}}: CS1 maint: unflagged free DOI (link)
  4. ^ Johnson, H. M.; Wright, C. D. (1983). "Predicted infrared brightness of stars within 25 parsecs of the sun". The Astrophysical Journal Supplement Series. 53: 643–771. Bibcode:1983ApJS...53..643J. doi:10.1086/190905.
  5. ^ Flower, Phillip J. (September 1996). "Transformations from Theoretical Hertzsprung-Russell Diagrams to Color-Magnitude Diagrams: Effective Temperatures, B-V Colors, and Bolometric Corrections". The Astrophysical Journal. 469: 355. Bibcode:1996ApJ...469..355F. doi:10.1086/177785.
  6. ^ Torres, Guillermo (November 2010). "On the Use of Empirical Bolometric Corrections for Stars". The Astronomical Journal. 140 (5): 1158–1162. arXiv:1008.3913. Bibcode:2010AJ....140.1158T. doi:10.1088/0004-6256/140/5/1158. {{cite journal}}: Unknown parameter |layurl= ignored (help)
  7. ^ Interpolated value from NASA Exoplanet Archive, per: Bessell, M. S. (1995). "The Temperature Scale for Cool Dwarfs". In Tinney, C. G. (ed.). The Bottom of the Main Sequence - and Beyond, Proceedings of the ESO Workshop. Springer-Verlag. p. 123. Bibcode:1995bmsb.conf..123B. {{cite conference}}: Unknown parameter |booktitle= ignored (|book-title= suggested) (help)
  8. ^ 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.
  9. ^ Safonova, M.; Murthy, J.; Shchekinov, Yu. A. (2014). "Age Aspects of Habitability". International Journal of Astrobiology. 15 (2): 93–105. arXiv:1404.0641. Bibcode:2016IJAsB..15...93S. doi:10.1017/S1473550415000208.
  10. ^ "Gliese 832". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-09-23.
  11. ^ "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
  12. ^ 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, A35.
  13. 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.
  14. 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.


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