HD 117207
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Centaurus |
| Right ascension | 13h 29m 21.11291s[1] |
| Declination | −35° 34′ 15.5880″[1] |
| Apparent magnitude (V) | 7.240[2] |
| Characteristics | |
| Spectral type | G7IV-V[3] |
| B−V color index | 0.727±0.014[2] |
| Astrometry | |
| 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) | 30.9440 ± 0.0256 mas[1] |
| Distance | 105.40 ± 0.09 ly (32.32 ± 0.03 pc) |
| Absolute magnitude (MV) | 4.67[4] |
| Details[2] | |
| Mass | 1.053±0.028 M☉ |
| Radius | 1.074±0.041 R☉ |
| Luminosity | 1.163+0.002 −0.003[5] L☉ |
| Surface gravity (log g) | 4.371±0.039 cgs |
| Temperature | 5,732±53 K |
| Metallicity [Fe/H] | 0.19±0.03 dex |
| Age | 4.192±2.274[2] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
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 axis of 3.79 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]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (years) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 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 −12.0 or 103.4+12.0 −9.3° |
— |
See also
[edit]References
[edit]- ^ a b c d 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.
- ^ a b c d e f g Barbato, D.; et al. (August 2018). "Exploring the realm of scaled solar system analogues with HARPS". Astronomy & Astrophysics. 615: 21. arXiv:1804.08329. Bibcode:2018A&A...615A.175B. doi:10.1051/0004-6361/201832791. S2CID 119099721. A175.
- ^ a b Gray, R. O.; et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 parsecs: The Northern Sample I". The Astronomical Journal. 132 (1): 161–170. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637. S2CID 119476992.
- ^ a b c d 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.
- ^ a b c 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.
- ^ "HD 117207". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-23.
- ^ Luck, R. Earle (March 2018). "Abundances in the Local Region. III. Southern F, G, and K Dwarfs". The Astronomical Journal. 155 (3): 31. Bibcode:2018AJ....155..111L. doi:10.3847/1538-3881/aaa9b5. S2CID 125765376. 111.
- ^ Marcy, Geoffrey W.; et al. (2005). "Five New Extrasolar Planets". The Astrophysical Journal. 619 (1): 570–584. Bibcode:2005ApJ...619..570M. CiteSeerX 10.1.1.516.6667. doi:10.1086/426384. S2CID 5803173.
- ^ Butler, R. P.; et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal. 646 (1): 505–522. arXiv:astro-ph/0607493. Bibcode:2006ApJ...646..505B. doi:10.1086/504701. S2CID 119067572.
- ^ a b Xiao, Guang-Yao; Liu, Yu-Juan; et al. (May 2023). "The Masses of a Sample of Radial-Velocity Exoplanets with Astrometric Measurements". Research in Astronomy and Astrophysics. 23 (5): 055022. arXiv:2303.12409. Bibcode:2023RAA....23e5022X. doi:10.1088/1674-4527/accb7e.
