Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Draco |
Right ascension | 17h 25m 24.055s [1] |
Declination | 52° 47′ 26.47″ [1] |
Apparent magnitude (V) | 6.46 [2] |
Characteristics | |
HD 158259 | |
Evolutionary stage | Main sequence |
Spectral type | G0 [2] (G5VmF9 [3]) |
Astrometry | |
Radial velocity (Rv) | 13.44±0.14 [1] km/s |
Proper motion (μ) |
RA: −90.678
[1]
mas/
yr Dec.: −49.702 [1] mas/ yr |
Parallax (π) | 37.0177 ± 0.0199 mas [1] |
Distance | 88.11 ± 0.05
ly (27.01 ± 0.01 pc) |
Absolute magnitude (MV) | 4.27 [4] |
Details | |
Mass | 0.985 [1] M☉ |
Radius | 1.3 [1] R☉ |
Luminosity | 1.6 [1] L☉ |
Surface gravity (log g) | 4.28 [5] cgs |
Temperature | 6,068 [5] K |
Metallicity [Fe/H] | −0.20 [5] dex |
Rotation | 18 days [2] |
Rotational velocity (v sin i) | 3.0 [6] km/s |
Other designations | |
HIP 85268, 2MASS J17252406+5247263, TYC 3888-1886-1, TOI-1462, GSC 03888-01886
[7] | |
Database references | |
SIMBAD | data |
Exoplanet Archive | data |
HD 158259 is a main sequence star located 88 light-years (27 parsecs) away in the constellation Draco. It hosts a system of at least five planets, discovered by the SOPHIE échelle spectrograph using the radial velocity method. [2]
HD 158259 is a G0 star with a rotation period of 18±5 days. More detailed analysis of the spectral assigns a class of G5V, but with the metal lines of an F9 star. [3]
Five planets have been confirmed orbiting HD 158259, along with one unconfirmed planet. These planets were discovered by N.C. Hara et.al. by the radial velocity method, published in Astronomy & Astrophysics in April 2020. [8] The innermost planet, HD 158259 b, was also observed to transit the star by TESS. [2] The planets orbit in a nearly 3:2 orbital resonance, with the period ratios 1.5758, 1.5146, 1.5296, 1.5130, and 1.4480, respectively, starting from the innermost pairing. [9] A dynamical analysis has shown that the system is stable. [2] One of the planets, HD 158259 b, is a super-Earth; the rest, including the unconfirmed HD 158259 g, are mini-Neptunes. [8]
Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b | 2.2 M🜨 | 0.034 | 2.177±0.44 | <0.1 | — | ~1.2 R🜨 |
c | 5.6 M🜨 | 0.046 | 3.432±0.00002 | <0.1 | — | — |
d | 5.4 M🜨 | 0.060 | 5.198±0.008 | <0.1 | — | — |
e | 6.1 M🜨 | 0.080 | 7.954±0.0016 | <0.1 | — | — |
f | 6.1 M🜨 | 0.105 | 12.03±0.0028 | <0.1 | — | — |
g (unconfirmed) | 6.9 M🜨 | 0.135 | 17.39±0.023 | <0.1 | — | — |
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Draco |
Right ascension | 17h 25m 24.055s [1] |
Declination | 52° 47′ 26.47″ [1] |
Apparent magnitude (V) | 6.46 [2] |
Characteristics | |
HD 158259 | |
Evolutionary stage | Main sequence |
Spectral type | G0 [2] (G5VmF9 [3]) |
Astrometry | |
Radial velocity (Rv) | 13.44±0.14 [1] km/s |
Proper motion (μ) |
RA: −90.678
[1]
mas/
yr Dec.: −49.702 [1] mas/ yr |
Parallax (π) | 37.0177 ± 0.0199 mas [1] |
Distance | 88.11 ± 0.05
ly (27.01 ± 0.01 pc) |
Absolute magnitude (MV) | 4.27 [4] |
Details | |
Mass | 0.985 [1] M☉ |
Radius | 1.3 [1] R☉ |
Luminosity | 1.6 [1] L☉ |
Surface gravity (log g) | 4.28 [5] cgs |
Temperature | 6,068 [5] K |
Metallicity [Fe/H] | −0.20 [5] dex |
Rotation | 18 days [2] |
Rotational velocity (v sin i) | 3.0 [6] km/s |
Other designations | |
HIP 85268, 2MASS J17252406+5247263, TYC 3888-1886-1, TOI-1462, GSC 03888-01886
[7] | |
Database references | |
SIMBAD | data |
Exoplanet Archive | data |
HD 158259 is a main sequence star located 88 light-years (27 parsecs) away in the constellation Draco. It hosts a system of at least five planets, discovered by the SOPHIE échelle spectrograph using the radial velocity method. [2]
HD 158259 is a G0 star with a rotation period of 18±5 days. More detailed analysis of the spectral assigns a class of G5V, but with the metal lines of an F9 star. [3]
Five planets have been confirmed orbiting HD 158259, along with one unconfirmed planet. These planets were discovered by N.C. Hara et.al. by the radial velocity method, published in Astronomy & Astrophysics in April 2020. [8] The innermost planet, HD 158259 b, was also observed to transit the star by TESS. [2] The planets orbit in a nearly 3:2 orbital resonance, with the period ratios 1.5758, 1.5146, 1.5296, 1.5130, and 1.4480, respectively, starting from the innermost pairing. [9] A dynamical analysis has shown that the system is stable. [2] One of the planets, HD 158259 b, is a super-Earth; the rest, including the unconfirmed HD 158259 g, are mini-Neptunes. [8]
Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b | 2.2 M🜨 | 0.034 | 2.177±0.44 | <0.1 | — | ~1.2 R🜨 |
c | 5.6 M🜨 | 0.046 | 3.432±0.00002 | <0.1 | — | — |
d | 5.4 M🜨 | 0.060 | 5.198±0.008 | <0.1 | — | — |
e | 6.1 M🜨 | 0.080 | 7.954±0.0016 | <0.1 | — | — |
f | 6.1 M🜨 | 0.105 | 12.03±0.0028 | <0.1 | — | — |
g (unconfirmed) | 6.9 M🜨 | 0.135 | 17.39±0.023 | <0.1 | — | — |