| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Sagittarius |
| Right ascension | 20 07 19.6698 |
| Declination | −35° 32′ 19.0786″ |
| Apparent magnitude (V) | 7.78 |
| Characteristics | |
| Spectral type | G5V |
| B−V color index | 0.743±0.002 |
| Variable type | Constant |
| Astrometry | |
| Radial velocity (Rv) | −40.33±0.12 km/s |
| Proper motion (μ) | RA: −26.622±0.079 mas/yr Dec.: −206.859±0.053 mas/yr |
| Parallax (π) | 18.3287 ± 0.0495 mas |
| Distance | 177.9 ± 0.5 ly (54.6 ± 0.1 pc) |
| Absolute magnitude (MV) | 4.00 |
| Details | |
| Mass | 1.07±0.01 M☉ |
| Radius | 1.56±0.03 R☉ |
| Luminosity | 2.19±0.01 L☉ |
| Surface gravity (log g) | 4.07±0.02 cgs |
| Temperature | 5,630+48 −40 K |
| Metallicity | 0.23 dex |
| Rotational velocity (v sin i) | 1.576 km/s |
| Age | 8.7±0.4 Gyr |
| Other designations | |
| CD–35°13924, HD 190647, HIP 99115, SAO 211821, LTT 7948, NLTT 48727, TYC 7449-1245-1, 2MASS J20071966-3532189 | |
| Database references | |
| SIMBAD | data |
HD 190647 is a yellow-hued star with an exoplanetary companion, located in the southern constellation of Sagittarius. It has an apparent visual magnitude of 7.78, making this an 8th magnitude star that is much too faint to be readily visible to the naked eye. The star is located at a distance of 178 light years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −40 km/s. It is also called HIP 99115.
The stellar classification of this star is G5V, matching a G-type main-sequence star. However, the low gravity and high luminosity of this star may indicate it is slightly evolved. It is chrompsherically inactive with a slow rotation, having a projected rotational velocity of 1.6 km/s. The star's metallicity is high, with nearly 1.5 times the abundance of iron compared to the Sun.
In 2007, a Jovian planet was found to be orbiting the star. It was detected using the radial velocity method with the HARPS spectrograph in Chile. The object is orbiting at a distance of 2.0 AU from the host star with a period of 2.84 years and an eccentricity (ovalness) of 0.18. As the inclination of the orbital plane is unknown, only a lower bound on the planetary mass can be made. It has a minimum mass 1.9 times the mass of Jupiter.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >1.9 ± 0.06 MJ | 2.07 ± 0.06 | 1038.1 ± 4.9 | 0.18 ± 0.02 | — | — |
See also
References
- ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ 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.
- ^ Houk, Nancy (1979). Michigan catalogue of two-dimensional spectral types for the HD stars. Vol. 3. Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan. Bibcode:1982mcts.book.....H.
- ^ Naef, M.; et al. (2007). "The HARPS search for southern extra-solar planets. IX. Exoplanets orbiting HD 100777, HD 190647, and HD 221287". Astronomy and Astrophysics. 470 (2): 721–726. arXiv:0704.0917. Bibcode:2007A&A...470..721N. doi:10.1051/0004-6361:20077361.
- ^ Bonfanti, A.; Ortolani, S.; Nascimbeni, V. (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.
- ^ Costa Silva, A. R.; et al. (February 2020). "Chemical abundances of 1111 FGK stars from the HARPS-GTO planet search sample. III. Sulfur". Astronomy & Astrophysics. 634: 10. arXiv:1912.08659. Bibcode:2020A&A...634A.136C. doi:10.1051/0004-6361/201936523. S2CID 209405391. A136.
- "HD 190647". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-11-11.
