Astronomy:HD 4313
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Pisces[1] |
| Right ascension | 00h 45m 40.3578s[2] |
| Declination | +07° 50′ 42.075″[2] |
| Apparent magnitude (V) | 7.83[1] |
| Characteristics | |
| Evolutionary stage | subgiant[3] |
| Spectral type | G5[4] |
| B−V color index | +0.963±0.017[1] |
| Astrometry | |
| Radial velocity (Rv) | +14.48±0.23[1] km/s |
| Proper motion (μ) | RA: −6.281[2] mas/yr Dec.: +6.566[2] mas/yr |
| Parallax (π) | 7.3090 ± 0.0879[2] mas |
| Distance | 446 ± 5 ly (137 ± 2 pc) |
| Absolute magnitude (MV) | 2.17[1] |
| Details | |
| Mass | 1.61+0.13−0.12[5] M☉ |
| Radius | 5.15+0.18−0.17[6] R☉ |
| Luminosity | 15.81[1] L☉ |
| Surface gravity (log g) | 3.24[7] cgs |
| Temperature | 4,966±40[6] K |
| Metallicity [Fe/H] | 0.05±0.10[6] dex |
| Rotational velocity (v sin i) | 1.91±0.25[7] km/s |
| Age | 2.03+0.64−0.45[6] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 4313 is a star with an orbiting exoplanetary companion in the constellation of Pisces. It has an apparent visual magnitude of 7.83,[1] which is too faint to be reading visible to the unaided eye. The system is located at a distance of 446 light years based on parallax, and is drifting further away with a radial velocity of 14.5 km/s.[1] This is a single star, which means it has no binary partners, at least in a range of projected separations from 6.85 to 191.78 AU.[9] It hosts an extrasolar planet.
This is an aging G-type star with a mass of nearly twice the Sun, although different methods give mass estimates which differ as much as 0.5 M☉.[6] It is a swollen star with 5.14 times the radius of the Sun, and has a cool effective temperature of 4,966±40 k. It is a G-type subgiant star[3] which has exhausted the hydrogen at its core, and is cooling and expanding to become a red giant. It is around two billion years in age and is spinning with a projected rotational velocity of 1.9 km/s.
Planetary system
HD 4313 has a superjovian exoplanet orbiting it. This exoplanet was discovered in 2010.[10] It is orbiting the star at a distance of 1.16 astronomical unit|AU with an orbital period of 356 days and an eccentricity (ovalness) of 0.15. As the orbital inclination is unknown, only a lower bound on the mass can be determined. The exoplanet has at least 1.2 times the mass of Jupiter.[3]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A XHIP record for this object at VizieR.
- ↑ 2.0 2.1 2.2 2.3 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 3.3 Luhn, Jacob K. et al. (2019). "Retired A Stars and Their Companions. VIII. 15 New Planetary Signals around Subgiants and Transit Parameters for California Planet Search Planets with Subgiant Hosts". The Astronomical Journal 157 (4): 149. doi:10.3847/1538-3881/aaf5d0. Bibcode: 2019AJ....157..149L.
- ↑ Cannon, A. J.; Pickering, E. C. (1993). "VizieR Online Data Catalog: Henry Draper Catalogue and Extension (Cannon+ 1918-1924; ADC 1989)". Vizier Online Data Catalog. Bibcode: 1993yCat.3135....0C.
- ↑ Malla, Sai Prathyusha; Stello, Dennis; Huber, Daniel; Montet, Benjamin T.; Bedding, Timothy R.; Fredslund Andersen, Mads; Grundahl, Frank; Jessen-Hansen, Jens et al. (2020). "Asteroseismic masses of four evolved planet-hosting stars using SONG and TESS: Resolving the retired A-star mass controversy". Monthly Notices of the Royal Astronomical Society 496 (4): 5423–5435. doi:10.1093/mnras/staa1793.
- ↑ 6.0 6.1 6.2 6.3 6.4 North, Thomas S. H.; Campante, Tiago L.; Miglio, Andxsrea; Davies, Guy R.; Grunblatt, Samuel K.; Huber, Daniel; Kuszlewicz, James S.; Lund, Mikkel N. et al. (2017). "The masses of retired a stars with asteroseismology: Kepler and K2 observations of exoplanet hosts". Monthly Notices of the Royal Astronomical Society 472 (2): 1866–1878. doi:10.1093/mnras/stx2009.
- ↑ 7.0 7.1 "Exoplanet Archive". https://exoplanetarchive.ipac.caltech.edu/overview/HD%204313#star_HD-4313_collapsible.
- ↑ "HD 4313". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+4313.
- ↑ Wittrock, Justin M.; Kane, Stephen R.; Horch, Elliott P.; Howell, Steve B.; Ciardi, David R.; Everett, Mark E. (2017). "Exclusion of Stellar Companions to Exoplanet Host Stars". The Astronomical Journal 154 (5): 184. doi:10.3847/1538-3881/aa8d69. Bibcode: 2017AJ....154..184W.
- ↑ Johnson, John Asher; Howard, Andrew W.; Bowler, Brendan P.; Henry, Gregory W.; Marcy, Geoffrey W.; Wright, Jason T.; Fischer, Debra A.; Isaacson, Howard (2010). "Retired a Stars and Their Companions. IV. Seven Jovian Exoplanets from Keck Observatory1". Publications of the Astronomical Society of the Pacific 122 (892): 701–711. doi:10.1086/653809. Bibcode: 2010PASP..122..701J.
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