HD 23127

HD 23127 is a star in the southern constellation of Reticulum. With an apparent visual magnitude of +8.58[4] it is not visible to the naked eye, but can be viewed with a good pair of binoculars. The star is located at a distance of 307 light years from the Sun based on parallax, and is drifting further away with a radial velocity of ~22 km/s.[4] It has an absolute magnitude of 3.62.[4]

HD 23127
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Reticulum
Right ascension 03h 39m 23.63799s[1]
Declination −60° 04′ 40.2386″[1]
Apparent magnitude (V) +8.576±0.002[2]
Characteristics
Spectral type G2V[3]
B−V color index 0.701±0.013[2]
Astrometry
Radial velocity (Rv)+21.9±1.7[4] km/s
Proper motion (μ) RA: 73.621±0.042[1] mas/yr
Dec.: 142.847±0.045[1] mas/yr
Parallax (π)10.6258 ± 0.0232 mas[1]
Distance306.9 ± 0.7 ly
(94.1 ± 0.2 pc)
Absolute magnitude (MV)3.62[4]
Details[2]
Mass1.208±0.045 M☉
Radius1.490±0.104 R☉
Luminosity3.01±0.03[5] L☉
Surface gravity (log g)4.146±0.054 cgs
Temperature5,843±52 K
Metallicity [Fe/H]0.29±0.03 dex
Rotation~33 days
Age4.508±0.788 Gyr
Other designations
CD−60°762, HD 23127, HIP 17054, SAO 248860, TYC 8867-913-1, GSC 08867-00913[6]
Database references
SIMBADdata

This is a G-type main-sequence star with a stellar classification of G2V,[3] which means it is generating energy through core hydrogen fusion. HD 23127 is more massive than the Sun at 1.21 solar masses and has a 49% larger radius. It is metal-rich, having nearly double the abundance of iron in its atmosphere compared to the Sun. This star has an age of 4.5 billion years;[2] about the same as the Sun.

On Friday, February 9, 2007, a 3.32 years period jovian planet was found by using the wobble method by O'Toole and colleagues in Australia.[7] It has minimum mass 53% greater than Jupiter and orbits with a 41% eccentricity. The maximum stable period for a hypothetical inner planet is 322.1 days.[2]

The HD 23127 planetary system[2]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥1.527+0.037
−0.038 MJ		 2.370±0.032 1,211.17+11.11
−8.91		 0.406+0.083
−0.09		 — —

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. Barbato, D.; et al. (August 2018). "Exploring the realm of scaled solar system analogues with HARPS". Astronomy & Astrophysics. 615: 21. arXiv:1804.08329. Bibcode:2018A&A...615A.175B. doi:10.1051/0004-6361/201832791. S2CID 119099721. A175.
  3. Houk, Nancy (1979). Michigan catalogue of two-dimensional spectral types for the HD stars. Vol. 1. Ann Arbor, Michigan: Department of Astronomy, University of Michigan. Bibcode:1978mcts.book.....H.
  4. 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.
  5. Bonfanti, A.; et al. (2015). "Revising the ages of planet-hosting stars". Astronomy and Astrophysics. 575. A18. arXiv:1411.4302. Bibcode:2015A&A...575A..18B. doi:10.1051/0004-6361/201424951.
  6. "HD 23127". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-08-15.
  7. O'Toole, Simon J.; et al. (2007). "New Planets around Three G Dwarfs". The Astrophysical Journal. 660 (2): 1636–1641. arXiv:astro-ph/0702213. Bibcode:2007ApJ...660.1636O. doi:10.1086/513563.
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.