HD 212301

HD 212301 is a binary star[4] system in the south circumpolar constellation of Octans. This star is also called HIP 110852.[7] With an apparent visual magnitude of 7.76,[2] it is too faint to be visible to the naked eye. The system is located at a distance of 177 light years from the Sun based on parallax,[1] and is drifting further away with a radial velocity of +4.7 km/s.[2] It has an absolute magnitude of 4.06.[2]

HD 212301
Observation data
Epoch J2000      Equinox J2000
Constellation Octans
Right ascension 22h 27m 30.92159s[1]
Declination −77° 43′ 04.5298″[1]
Apparent magnitude (V) 7.76[2]
Characteristics
Spectral type F8V[3] + M3V[4]
B−V color index 0.560±0.010[2]
Astrometry
Radial velocity (Rv)+4.69±0.01[2] km/s
Proper motion (μ) RA: 76.862±0.051[1] mas/yr
Dec.: −92.203±0.055[1] mas/yr
Parallax (π)18.4109 ± 0.0290[1] mas
Distance177.2 ± 0.3 ly
(54.32 ± 0.09 pc)
Absolute magnitude (MV)4.06[2]
Details
A
Mass1.20[5] M☉
Radius1.23+0.04
−0.02[1] R☉
Luminosity1.911±0.005[1] L☉
Surface gravity (log g)4.35[5] cgs
Temperature6169±37[5] K
Metallicity [Fe/H]0.13±0.02[2] dex
Rotational velocity (v sin i)5.44[6] km/s
Age4.2+1.1
−1.4[2] Gyr
B
Mass0.35±0.02[4] M☉
Other designations
CPD−78° 1011, GC 31330, HD 212301, HIP 110852, SAO 258040, WDS J20379-6038AB[7]
Database references
SIMBADdata
Extrasolar Planets
Encyclopaedia		data

The primary, component A, is an F-type main-sequence star with a stellar classification of F8V.[3] It has 20%[5] greater mass than the Sun and a 23%[1] larger radius. Its age is about the same as the Sun and it is spinning with a projected rotational velocity of 5.4 km/s.[6] It is a metal-rich star with 50% more metals than the Sun has.[6] The star is radiating 1.9[1] times the luminosity of the Sun from its photosphere at an effective temperature of 6,169 K.[1]

A secondary companion was announced in 2009. This faint star is located at an angular separation of 4.4″ to the northwest of the primary, corresponding to a projected separation of ~230 AU. This is a red dwarf with an estimated class of M3V and a mass equal to around 35% of the mass of the Sun. The pair share a common proper motion.[4]

A hot jupiter candidate exoplanet was discovered orbiting the primary, based on radial velocity observations taken in 2003 and 2005.[6]

The HD 212301 planetary system[6]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b >0.45 MJ 0.036 2.245715±0.000028 0.0 (fixed) — —

See also

References
  1. 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.
  2. 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.
  3. Houk, Nancy (1979). Michigan catalogue of two-dimensional spectral types for the HD stars. 1. Ann Arbor, Michigan: Department of Astronomy, University of Michigan. Bibcode:1978mcts.book.....H.
  4. Mugrauer, M.; Neuhäuser, R. (January 2009). "The multiplicity of exoplanet host stars. New low-mass stellar companions of the exoplanet host stars HD 125612 and HD 212301". Astronomy and Astrophysics. 494 (1): 373–378. arXiv:0812.2561. Bibcode:2009A&A...494..373M. doi:10.1051/0004-6361:200810639. S2CID 15018915.
  5. 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. 111.
  6. Lo Curto, G.; et al. (2006). "The HARPS search for southern extra-solar planets VII. A very hot Jupiter orbiting HD 212301". Astronomy & Astrophysics. 451 (1): 345–350. Bibcode:2006A&A...451..345L. doi:10.1051/0004-6361:20054083.
  7. "HD 212301". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-27.

This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.