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==Planetary system== ==Planetary system==


Gliese 832 hosts two known planets.
⚫ In September 2008, it was announced that a ]-like planet 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. Among currently-known exoplanets, it would have an ] from its star second only to ], although direct imaging is problematic due to the star–planet contrast.<ref name="bailey08" />

⚫ In September 2008, it was announced that a ]-like planet 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 super-Earth mass planet was announced to orbit in the optimistic habitable zone but outside the conservative habitable zone.<ref name="Wittenmyer14" />


If this system has a comet disc, it is undetectable "brighter than the fractional dust luminosity 10<sup>−5</sup>" of a recent Herschel study.<ref name=nodebris/> If this system has a comet disc, it is undetectable "brighter than the fractional dust luminosity 10<sup>−5</sup>" of a recent Herschel study.<ref name=nodebris/>


{{OrbitboxPlanet begin}} {{OrbitboxPlanet begin}}
{{OrbitboxPlanet
| exoplanet = ]
| mass_earth = ≥5.4±1
| period = 35.68±0.03
| semimajor =
| eccentricity = 0.18 ± 0.13
}}
{{OrbitboxPlanet {{OrbitboxPlanet
| exoplanet = ] | exoplanet = ]
Line 119: Line 130:
|bibcode=2009ApJ...690..743B |bibcode=2009ApJ...690..743B
|doi=10.1088/0004-637X/690/1/743 |doi=10.1088/0004-637X/690/1/743
}}</ref>

<ref name="Wittenmyer14">
{{cite journal
|last1=Wittenmyer |first1=R.A.
|last2=Tuomi |first2=M.
|last3=Butler |first3=R.P.
|last4=Jones |first4=H. R. A.
|last5=O'Anglada-Escude |first5=G.
|last6=Horner |first6=J.
|last7=Tinney |first7=C.G.
|last8=Marshall |first7=J.P.
|last9=Carter |first7=B.D.
|year=2014
|title= GJ 832c: A super-earth in the habitable zone
|journal=
|arxiv=1406.5587
}}</ref> }}</ref>


Revision as of 05:04, 24 June 2014

Gliese 832
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Grus
Right ascension 21 33 33.975
Declination −49° 00′ 32.42″
Apparent magnitude (V) 8.66
Characteristics
Spectral type M1.5V
B−V color index 1.52
Astrometry
Radial velocity (Rv)18.0 km/s
Proper motion (μ) RA: −46.05 ± 0.95 mas/yr
Dec.: −817.63 ± 0.59 mas/yr
Parallax (π)201.87 ± 1.01 mas
Distance16.16 ± 0.08 ly
(4.95 ± 0.02 pc)
Details
Mass0.45 ± 0.05 M☉
Radius0.48 R☉
Luminosity (bolometric)0.035 L☉
Surface gravity (log g)4.7 cgs
Temperature3,620 K
Metallicity−0.31 ± 0.2
Other designations
HD 204961, HIP 106440, LHS 3865
Database references
SIMBADdata
Exoplanet Archivedata
Data sources:
Hipparcos Catalogue,
HD

Gliese 832 (Gl 832 or GJ 832) is a red dwarf (spectrum M1.5V) in the constellation Grus. It is located relatively close to the Sun, at a distance of 16.1 light years. Gliese 832 has about half the mass and radius of the Sun.

Planetary system

Gliese 832 hosts two known planets.

In September 2008, it was announced that a Jupiter-like planet 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 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.

In 2014, a second super-Earth mass planet was announced to orbit in the optimistic habitable zone but outside the conservative habitable zone.

If this system has a comet disc, it is undetectable "brighter than the fractional dust luminosity 10" of a recent Herschel study.

The Gliese 832 planetary system
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
c ≥5.4±1 M🜨 — 35.68±0.03 0.18 ± 0.13 — —
b ≥0.64 ± 0.06 MJ 3.4 ± 0.4 3416 ± 131 0.12 ± 0.11 — —

X-ray source

Gliese 832 emits X-rays.

See also

Notes

  1. From L = 4πRσTeff, where L is the luminosity, R is the radius, Teff is the effective surface temperature and σ is the Stefan–Boltzmann constant.

References

  1. ^ van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction" (PDF). Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. Vizier catalog entry
  2. ^ Bailey, J.; Butler, R. P.; Tinney, C. G.; Jones, H. R. A.; O'Toole, S.; Carter, B. D.; Marcy, G. W. (2008). "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. 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.
  4. 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)
  5. Wittenmyer, R.A.; Tuomi, M.; Butler, R.P.; Jones, H. R. A.; O'Anglada-Escude, G.; Horner, J.; Tinney, B.D.; Marshall; Carter (2014). "GJ 832c: A super-earth in the habitable zone". arXiv:1406.5587. {{cite journal}}: Cite journal requires |journal= (help)
  6. B. C. Matthews; forthcoming study promised in Lestrade, J.-F.; et al. (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. {{cite journal}}: Explicit use of et al. in: |author2= (help)
  7. 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.
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
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Variable
HR
HD
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Exoplanets
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