13h29m21.1137s, −35° 34′ 15.589″13h29m 21.11291s[1]
−35° 34′ 15.5880″[1]
7.240[2]
Characteristics
G7IV-V[3]
B−V color index
0.727±0.014[2]
Radial velocity (Rv)
−17.43±0.09[4] km/s
Proper motion (μ)
RA: −205.904 mas/yr[1]
Dec.: −71.402 mas/yr[1]
Parallax (π)
105.40 ± 0.09 ly
(32.32 ± 0.03 pc)
Absolute magnitude (MV)
4.67[4]
Details[2]
1.053±0.028 M☉
1.074±0.041 R☉
Surface gravity (log g)
4.371±0.039 cgs
5,732±53 K
Metallicity [Fe/H]
0.19±0.03 dex
Database references
HD 117207 is a star in the southern constellation Centaurus. With an apparent visual magnitude of 7.24,[2] it is too dim to be visible to the naked eye but can be seen with a small telescope. Based upon parallax measurements, it is located at a distance of 105.4 light-years (32.3 parsecs) from the Sun. The star is drifting closer with a radial velocity of −17.4 km/s.[4] It has an absolute magnitude of 4.67.[4]
This object has a stellar classification of G7IV-V,[3] showing blended spectral traits of a G-type main-sequence star and an older, evolving subgiant star. It is around four[2] billion years old with 5%[7] greater mass than the Sun and a 7% larger radius.[5] The star is radiating 1.16 times the luminosity of the Sun from its photosphere at an effective temperature of 5,644 K.[5]
In 2005, a planet was found orbiting the star using the radial velocity method, and was designated HD 117207 b.[8][9] The orbital elements of this planet were refined in 2018, showing an orbital period of 7.18 years, a semimajor axisof3.79 AU, and an eccentricity of 0.16. The minimum mass of this object is nearly double that of Jupiter. If an inner planet is orbiting the star, it must have an orbital period no greater than 3.46 years to satisfy Hill's criteria for dynamic stability.[2] In 2023, the inclination and true mass of HD 117207 b were determined via astrometry.[10]
The HD 117207 planetary system[10]
Companion
(in order from star)
2.106+0.16
−0.089 MJ
3.773+0.036
−0.035
7.136+0.034
−0.035
0.04+0.026
−0.024
76.6+9.3
−12.0or103.4+12.0
−9.3°
—
Other
Other
