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Revision as of 03:59, 23 September 2012 by 99.250.86.193 (talk) (→X-ray source)(diff) ← Previous revision | Latest revision (diff) | Newer revision → (diff)Observation data Epoch J2000.0 Equinox J2000.0 | |
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Constellation | Grus |
Right ascension | 21 33 33.9752 |
Declination | −49° 00′ 32.422″ |
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: -46.18 mas/yr Dec.: -817.96 mas/yr |
Parallax (π) | 202.52 ± 1.33 mas |
Distance | 16.1 ± 0.1 ly (4.94 ± 0.03 pc) |
Details | |
Mass | 0.45 ± 0.05 M☉ |
Radius | 0.48 R☉ |
Luminosity (bolometric) | 0.035 L☉ |
Surface gravity (log g) | 4.7 cgs |
Temperature | 3,620 K |
Metallicity | −0.31 ± 0.2 |
Other designations | |
HD 204961, HIP 106440, LHS 3865 | |
Database references | |
SIMBAD | data |
Exoplanet Archive | data |
Data sources: | |
Hipparcos Catalogue, HD |
Gliese 832 (Gl 832 or GJ 832) is a red dwarf star (spectrum M1.5V) in the constellation Grus. It is located relatively near our Sun, at a distance of 16.1 light years. The star is about half the mass and radius of the Sun.
Jupiter-like planet
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. Among currently-known exoplanets, it would have an angular distance from its star second only to Epsilon Eridani b, although direct imaging is problematic due to the star–planet contrast.
Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b | ≥0.64 ± 0.06 MJ | 3.4 ± 0.4 | 3416 ± 131 | 0.12 ± 0.11 | — | — |
X-ray source
Gliese 832 emits eX-rays.
See also
Notes
- 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
- ^ Bailey, Jeremy; et al. (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.
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(help); Explicit use of et al. in:|author=
(help) - ^ Perryman, M. A. C.; et al. (1997), "The Hipparcos Catalogue", Astronomy & Astrophysics, 323: L49 – L52, Bibcode:1997A&A...323L..49P
- Johnson, H. M.; Wright, C. D. (1983). "Predicted infrared brightness of stars within 25 parsecs of the sun". Astrophysical Journal Supplement Series. 53: 643–771. Bibcode:1983ApJS...53..643J. doi:10.1086/190905.
{{cite journal}}
: CS1 maint: multiple names: authors list (link) - Interpolated value from NASA Exoplanet Archive, per:
Bessell, M. S. (August 10–12, 1994). "The Bottom of the Main Sequence - and Beyond". Proceedings of the ESO Workshop. Garching, Germany: Springer-Verlag Berlin Heidelberg New York. Bibcode:1995bmsb.conf..123B.{{cite conference}}
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ignored (|editor=
suggested) (help)CS1 maint: date format (link) - 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". Astrophysical Journal. 450 (9): 392–400. Bibcode:1995ApJ...450..392S. doi:10.1086/176149.
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Italic are systems without known trigonometric parallax. |
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