HD 20367

HD 20367 is a star in the constellation of Aries, close to the border with the Perseus constellation. It is a yellow-white hued star that is a challenge to view with the naked eye, having an apparent visual magnitude of 6.40.[2] Based upon parallax measurements, it is located 85 light years from the Sun. It is drifting further away with a radial velocity of +6.4 km/s.[1] Based upon its movement through space, it is a candidate member of the Ursa Major Moving Group of co-moving stars that probably share a common origin.[7]

HD 20367
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Aries
Right ascension  03h 17m 40.04666s[1]
Declination +31° 07′ 37.3584″[1]
Apparent magnitude (V) 6.40[2]
Characteristics
Spectral type F8V[2]
B−V color index 0.574[2]
Astrometry
Radial velocity (Rv)+6.432±0.0027[1] km/s
Proper motion (μ) RA: −101.802[1] mas/yr
Dec.: −57.909[1] mas/yr
Parallax (π)38.2842 ± 0.0712[1] mas
Distance85.2 ± 0.2 ly
(26.12 ± 0.05 pc)
Absolute magnitude (MV)4.27[3]
Details
Mass1.13±0.10[4] M☉
Radius1.12+0.03
−0.01[1] R☉
Luminosity1.576±0.004[1] L☉
Surface gravity (log g)4.53±0.22[4] cgs
Temperature6,100+36
−60[1] K
Metallicity [Fe/H]0.17±0.10[4] dex
Rotational velocity (v sin i)5.5[5] km/s
Age2.98[5] Gyr
Other designations
BD+30°520, GC 3929, HD 20367, HIP 15323, SAO 56323[6]
Database references
SIMBADdata
Exoplanet Archivedata
Extrasolar Planets
Encyclopaedia		data

This object is a late F-type main-sequence star with a stellar classification of F8V.[2] It is about three[5] billion years old and is spinning with a projected rotational velocity of 5.5 km/s.[5] The star is 12%[1] larger and 13%[4] more massive than the Sun. It is radiating 1.58[1] times the luminosity of the Sun from its photosphere at an effective temperature of 6,100 K.[1]

Candidate planetary system

In June 2002, an announcement was made that a Jupiter-mass or larger extrasolar planet had been found orbiting the star,[8] with a period of 1.285 years and an eccentricity of 0.32. The eccentric nature of this planet's orbit meant that it spends part of each circuit around the star outside the habitable zone.[9] However, subsequent observations put the existence of this planet in doubt.[10]

The HD 20367 planetary system[11]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b >1.17 MJ 1.246±0.075 469.5±9.3 0.320±0.090 — —
gollark: Is that even Macron?
gollark: Fail.
gollark: Macron should have a compiler option to enable commutativity.
gollark: Wow, it's like one of those cluster leader election algorithms.
gollark: Oh bee oh apio forms.

See also
  • List of extrasolar planets

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. Abt, Helmut A. (November 2004), "Spectral Classification of Stars in A Supplement to the Bright Star Catalogue", The Astrophysical Journal Supplement Series, 155 (1): 175–177, Bibcode:2004ApJS..155..175A, doi:10.1086/423803
  3. 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.
  4. Santos, N. C.; et al. (August 2013), "SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs. I. New atmospheric parameters and masses for 48 stars with planets", Astronomy & Astrophysics, 556: 11, arXiv:1307.0354, Bibcode:2013A&A...556A.150S, doi:10.1051/0004-6361/201321286, A150.
  5. Luck, R. Earle (January 2017), "Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants", The Astronomical Journal, 153 (1): 19, arXiv:1611.02897, Bibcode:2017AJ....153...21L, doi:10.3847/1538-3881/153/1/21, 21.
  6. "HD 20367". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-12-22.
  7. Tabernero, H. M.; et al. (January 2017), "Chemical tagging of the Ursa Major moving group. A northern selection of FGK stars", Astronomy & Astrophysics, 597: 25, arXiv:1409.2348, Bibcode:2017A&A...597A..33T, doi:10.1051/0004-6361/201322526, A33.
  8. A 1.1 Jupiter-mass planet orbiting HD 20367, Geneva Observatory, October 7, 2002. Accessed on line October 1, 2008.
  9. Érdi, B.; et al. (October 2007), "Secondary resonances of co-orbital motions", Monthly Notices of the Royal Astronomical Society, 381 (1): 33–40, arXiv:0707.4650, Bibcode:2007MNRAS.381...33E, doi:10.1111/j.1365-2966.2007.12228.x.
  10. Wittenmyer, Robert A.; et al. (May 2009), "A Search for Multi-Planet Systems Using the Hobby-Eberly Telescope", The Astrophysical Journal Supplement, 182 (1): 97–119, arXiv:0903.0652, Bibcode:2009ApJS..182...97W, doi:10.1088/0067-0049/182/1/97.
  11. Table 3, Catalog of Nearby Exoplanets, R. P. Butler et al., The Astrophysical Journal 646, #1 (July 2006), pp. 505–522, Bibcode: 2006ApJ...646..505B, doi:10.1086/504701.

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