HD 207832

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HD 207832
Observation data
Epoch J2000      Equinox J2000
Constellation Piscis Austrinus
Right ascension 21h 52m 36.2810s[1]
Declination −26° 01′ 35.6133″[1]
Apparent magnitude (V) 8.79
Characteristics
Evolutionary stage main-sequence star
Spectral type G5V[2]
Astrometry
Radial velocity (Rv)-16.481±0.185[3] km/s
Proper motion (μ) RA: 129.310[3] mas/yr
Dec.: -143.132[3] mas/yr
Parallax (π)16.8897 ± 0.0151[3] mas
Distance193.1 ± 0.2 ly
(59.21 ± 0.05 pc)
Details[4]
Mass1.08±0.01 M
Radius0.97±0.02 R
Luminosity0.78±0.09[2] L
Surface gravity (log g)4.61±0.04 cgs
Temperature5764±15 K
Metallicity [Fe/H]0.17±0.01 dex
Rotation17.8 d[5]
Age0.74±0.62 Gyr
Other designations
CD−26 15858, HIP 107985, TYC 6589-761-1, GSC 06956-00378, 2MASS J21523626-2601352[1]
Database references
SIMBADdata

HD 207832 is a G-type main-sequence star. Its surface temperature is 5764±15 K.[4] HD 207832 is slightly enriched compared to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of 0.17±0.01 and is much younger at an age of 0.74±0.62 billion years. Kinematically, it belongs to the thin disk of the Milky Way.[4]

A multiplicity study in 2014 detected a candidate comoving stellar companion - a red dwarf star or brown dwarf with a spectral class M6.5, at a very wide projected separation of 38.57′ (2.0 light years)[6]

Planetary system[]

In 2012, two planets, named and , were discovered by the radial velocity method on wide, eccentric orbits.[5] The planetary system would remain stable even if the planetary orbits are coplanar.[7]

Although discovery of the inner planet was confirmed[2] in 2018, the discovery of both planets was suspected to be a false positive in 2020, as newer radial velocity data do not support the existence of the planets.[8]

The HD 207832 planetary system[2][5]
Companion
(in order from star)
Mass Semimajor axis
(AU)
Orbital period
(days)
Eccentricity Inclination Radius
(unconfirmed) ≥ 0.56±0.091 MJ 0.586±0.032 160.07±0.23 0.197±0.053
(unconfirmed) ≥0.73+0.18
−0.05
M
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