| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Draco |
| Right ascension | 17 12 23.204816 |
| Declination | +63° 21′ 07.531205″ |
| Apparent magnitude (V) | 8.167±0.013 |
| Characteristics | |
| Evolutionary stage | main-sequence |
| Spectral type | K0 or G6 |
| Apparent magnitude (R) | 7.60 |
| Apparent magnitude (G) | 7.8657 |
| Apparent magnitude (J) | 6.677±0.018 |
| B−V color index | 0.801±0.014 |
| Astrometry | |
| Radial velocity (Rv) | −20.144±0.161 km/s |
| Proper motion (μ) | RA: −1.879±0.024 mas/yr Dec.: 160.429±0.027 mas/yr |
| Parallax (π) | 27.6756 ± 0.0200 mas |
| Distance | 117.85 ± 0.09 ly (36.13 ± 0.03 pc) |
| Absolute magnitude (MV) | 5.25 |
| Details | |
| Mass | 0.93±0.02 M☉ |
| Radius | 0.94±0.02 R☉ |
| Luminosity | 0.70±0.01 L☉ |
| Surface gravity (log g) | 4.45±0.03 cgs |
| Temperature | 5,449±31 K |
| Metallicity | 0.14±0.01 dex |
| Rotational velocity (v sin i) | 2.51±1 km/s |
| Age | 7.4±2.2 Gyr |
| Other designations | |
| BD+63 1335, Gaia DR2 1631084478574318976, HD 156279, HIP 84171, SAO 17390, PPM 20265, NLTT 44404, TYC 4202-656-1, 2MASS J17122319+6321074 | |
| Database references | |
| SIMBAD | data |
HD 156279 is a star with a pair of orbiting exoplanets located in the northern constellation of Draco. It has various alternate designations, including HIP 84171 and BD+63 1335. Parallax measurements yield a distance of 118 light years from the Sun, but it is drifting closer with a radial velocity of −20 km/s. Despite an absolute magnitude of 5.25, at that distance the star is too faint to be visible to the naked eye with an apparent visual magnitude of 8.17. It is presumed to be a single star, as in 2019 all imaging surveys have failed to find any stellar companions.
The spectrum of HD 156279 has a stellar classification of G6 or K0, depending on the study. Hence it presents as an ordinary main sequence star of the late G-type or early K-type. The star has 93% of the mass of the Sun and 94% of the Sun's radius. HD 156279 is roughly seven billion years old and is spinning with a projected rotational velocity of 2.5 km/s. Based on the abundance of iron, this star is slightly enriched in heavy elements, having 140% of the solar abundance. It is radiating 70% of the luminosity of the Sun from its photosphere at an effective temperature of 5,449 K.
Planetary system
Orbiting HD 156279 are two superjovian planets, the inner HD 156279 b (discovered in 2011) and outer HD 156279 c (discovered in 2016). In 2022, the inclination and true mass of HD 156279 c were measured via astrometry.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥ 9.50+0.31 −0.32 MJ |
0.5041+0.0082 −0.0085 |
133.4031+0.0037 −0.0040 |
0.64779+0.00068 −0.00066 |
— | — |
| c | 9.750+1.319 −0.605 MJ |
5.486+0.219 −0.240 |
4818.3+44.5 −43.1 |
0.261±0.006 | 74.699+36.999 −10.533° |
— |
References
- ^ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
- ^ Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ Biller, B.; et al. (2019), "A high binary fraction for the most massive close-in giant planets and brown dwarf desert members", Monthly Notices of the Royal Astronomical Society, 485 (4): 4967–4996, arXiv:1903.02332, Bibcode:2019MNRAS.485.4967F, doi:10.1093/mnras/stz671, S2CID 84180618.
- ^ Díaz, Rodrigo F.; et al. (2012), "The SOPHIE search for northern extrasolar planets IV. Massive companions in the planet-brown dwarf boundary", Astronomy & Astrophysics, A113: 538, arXiv:1111.1168, Bibcode:2012A&A...538A.113D, doi:10.1051/0004-6361/201117935, S2CID 55322205.
- ^ Carrera, R.; et al. (February 2022), "OCCASO. IV. Radial velocities and open cluster kinematics", Astronomy & Astrophysics, 658, arXiv:2110.02110, Bibcode:2022A&A...658A..14C, doi:10.1051/0004-6361/202141832, A14.
- ^ Bonfanti, A.; et al. (2016), "Age consistency between exoplanet hosts and field stars", Astronomy & Astrophysics, 585: 14, arXiv:1511.01744, Bibcode:2016A&A...585A...5B, doi:10.1051/0004-6361/201527297, S2CID 53971692, A5.
- "HD 156279". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 13 October 2020.
- ^ Bryan, Marta L.; et al. (2016), "Statistics of long period gas giant planets in known planetary systems", The Astrophysical Journal, 821 (2): 89, arXiv:1601.07595, Bibcode:2016ApJ...821...89B, doi:10.3847/0004-637X/821/2/89, S2CID 19709252.
- ^ Feng, Fabo; Butler, R. Paul; et al. (August 2022), "3D Selection of 167 Substellar Companions to Nearby Stars", The Astrophysical Journal Supplement Series, 262 (21): 21, arXiv:2208.12720, Bibcode:2022ApJS..262...21F, doi:10.3847/1538-4365/ac7e57, S2CID 251864022.
- "HD 156279 Overview", NASA Exoplanet Archive, California Institute of Technology, retrieved 2024-01-10.
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