HD 20367
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Aries |
| Right ascension | 03h 17m 40.04683s[1] |
| Declination | +31° 07′ 37.3604″[1] |
| Apparent magnitude (V) | 6.40[2] |
| Characteristics | |
| Spectral type | F8V[2] |
| B−V color index | 0.574[2] |
| Astrometry | |
| Radial velocity (Rv) | 6.47±0.15[1] km/s |
| Proper motion (μ) | RA: −101.950±0.031 mas/yr[1] Dec.: −58.033±0.028 mas/yr[1] |
| Parallax (π) | 38.3758 ± 0.0318 mas[1] |
| Distance | 84.99 ± 0.07 ly (26.06 ± 0.02 pc) |
| Absolute magnitude (MV) | 4.27[3] |
| Details | |
| Mass | 1.13±0.10[4] M☉ |
| Radius | 1.12+0.03 −0.01[5] R☉ |
| Luminosity | 1.576±0.004[5] L☉ |
| Surface gravity (log g) | 4.53±0.22[4] cgs |
| Temperature | 6,100+36 −60[5] K |
| Metallicity [Fe/H] | 0.17±0.10[4] dex |
| Rotational velocity (v sin i) | 5.5[6] km/s |
| Age | 2.98[6] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
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 +6.5 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.[8]
This object is a late F-type main-sequence star with a stellar classification of F8V.[2] It is about three[6] billion years old and is spinning with a projected rotational velocity of 5.5 km/s.[6] The star is 12%[5] larger and 13%[4] more massive than the Sun. It is radiating 1.58[5] times the luminosity of the Sun from its photosphere at an effective temperature of 6,100 K.[5]
Claims of a planetary system
[edit]In June 2002, an announcement was made that a Jupiter-mass or larger extrasolar planet had been found orbiting the star,[9] 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.[10] However, subsequent observations in 2009 put the existence of this planet in doubt.[11]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b (unconfirmed) | >1.17 MJ | 1.246±0.075 | 469.5±9.3 | 0.320±0.090 | — | — |
See also
[edit]References
[edit]- ^ a b c d e f 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 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
- ^ 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 d 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, S2CID 55237847, A150.
- ^ a b c d e f 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.
- ^ a b c d 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, S2CID 119511744, 21.
- ^ "HD 20367". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-12-22.
- ^ 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, S2CID 54819621, A33.
- ^ A 1.1 Jupiter-mass planet orbiting HD 20367, Geneva Observatory, October 7, 2002. Accessed on line October 1, 2008.
- ^ 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, S2CID 9742852.
- ^ 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, S2CID 7422668.
- ^ 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.
External links
[edit]- "HD 20367". Stars with exoplanets.
- HIP 15323 Catalog
- Image HD 20367
- Sky map
