HD 117618
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Centaurus |
| Right ascension | 13h 32m 25.55543s[1] |
| Declination | –47° 16′ 16.9091″[1] |
| Apparent magnitude (V) | 7.17[2] |
| Characteristics | |
| Spectral type | G0 V[3] |
| B−V color index | 0.603±0.010[2] |
| Astrometry | |
| Radial velocity (Rv) | +1.60±0.76[2] km/s |
| Proper motion (μ) | RA: +24.87[1] mas/yr Dec.: −125.01[1] mas/yr |
| Parallax (π) | 26.34 ± 0.60[1] mas |
| Distance | 124 ± 3 ly (38.0 ± 0.9 pc) |
| Absolute magnitude (MV) | 4.27[2] |
| Details[4] | |
| Mass | 1.10±0.02 M☉ |
| Radius | 1.17±0.04 R☉ |
| Luminosity | 1.6±0.1 L☉ |
| Surface gravity (log g) | 4.34±0.03 cgs |
| Temperature | 6,019±50 K |
| Metallicity [Fe/H] | +0.03±0.01[5] dex |
| Rotational velocity (v sin i) | 3.67[6] km/s |
| Age | 4.0±1.3 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Extrasolar Planets Encyclopaedia | data |
HD 117618 is a single,[8] yellow-hued star in the southern constellation of Centaurus. With an apparent visual magnitude of 7.17,[2] it is too faint to be visible to the naked eyes of a typical observer. The distance to this star, as determined from its annual parallax shift of 26.34±0.60 mas as seen from Earth's orbit,[1] is about 124 light years. It is moving further away with a heliocentric radial velocity of around +1.6 km/s.[2]
This star is similar to the Sun, being a G-type main-sequence star with a stellar classification of G0 V.[3] It is about 10% more massive and 17% larger than the Sun, with an estimated age of roughly four billion years[4] and a projected rotational velocity of 3.67 km/s.[6] The star is radiating 1.6 times the Sun's luminosity from its photosphere at an effective temperature of 6,019 K.[4]
In 2005, the Anglo-Australian Planet Search program announced the discovery of a low-mass planet in orbit around HD 117618. This object was found through measurements of radial velocity variation, which were larger than those produced by the intrinsic jitter of the host star. The best Keplerian fit to the data gave a periodicity of 25.8 days with an eccentricity of around 0.37 and a semimajor axis of 0.17 AU. The lower bound on the object's mass was estimated to be 0.16 MJ.[9] These values were subsequently refined, as shown in the table below.[10]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >0.178 ± 0.021 MJ | 0.176 ± 0.010 | 25.827±0.019 | 0.42 ± 0.17 | — | — |
See also
References
- 1 2 3 4 5 6 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357.
- 1 2 3 4 5 6 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.
- 1 2 Gray, R. O.; et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal. 132 (1): 161–170. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637.
- 1 2 3 Bonfanti, A.; Ortolani, S.; Nascimbeni, V. (2016). "Age consistency between exoplanet hosts and field stars". Astronomy & Astrophysics. 585: A5, 14 pp. arXiv:1511.01744. Bibcode:2016A&A...585A...5B. doi:10.1051/0004-6361/201527297.
- ↑ Adibekyan, V.; et al. (August 2016). "Abundance trend with condensation temperature for stars with different Galactic birth places". Astronomy & Astrophysics. 592: 12. arXiv:1606.04714. Bibcode:2016A&A...592A..87A. doi:10.1051/0004-6361/201628883. A87.
- 1 2 Delgado Mena, E.; et al. (April 2015). "Li abundances in F stars: planets, rotation, and Galactic evolution". Astronomy & Astrophysics. 576: 24. arXiv:1412.4618. Bibcode:2015A&A...576A..69D. doi:10.1051/0004-6361/201425433. A69.
- ↑ "HD 114837". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-05.
- ↑ Raghavan, Deepak; et al. (July 2006), "Two Suns in The Sky: Stellar Multiplicity in Exoplanet Systems", The Astrophysical Journal, 646 (1): 523–542, arXiv:astro-ph/0603836, Bibcode:2006ApJ...646..523R, doi:10.1086/504823.
- ↑ Tinney, C. G.; et al. (2005). "Three Low-Mass Planets from the Anglo-Australian Planet Search". The Astrophysical Journal. 623 (2): 1171–1179. Bibcode:2005ApJ...623.1171T. CiteSeerX 10.1.1.491.2941. doi:10.1086/428661.
- 1 2 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.
