51 Arietis

51 Arietis is a star in the northern constellation of Aries. 51 Arietis is the Flamsteed designation. It is a dim, yellow-hued star – a challenge to view with the naked eye, having an apparent visual magnitude of 6.6.[2] Based upon parallax measurements, the star is located at an estimated distance of 67.3 light-years (20.6 parsecs) from the Sun.[8] It is receding from the Earth with a heliocentric radial velocity of +9.5 km/s,[5] and is a member of the IC 2391 moving group.[3]

51 Arietis
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Aries
Right ascension 03h 02m 26.02628s[1]
Declination +26° 36′ 33.2602″[1]
Apparent magnitude (V) 6.623 ± 0.005[2]
Characteristics
Spectral type G8 V[3]
B−V color index 0.715[4]
Astrometry
Radial velocity (Rv)+9.5±0.1[5] km/s
Proper motion (μ) RA: +233.122[1] mas/yr
Dec.: –168.438[1] mas/yr
Parallax (π)47.1551 ± 0.0603 mas[1]
Distance69.17 ± 0.09 ly
(21.21 ± 0.03 pc)
Absolute bolometric
magnitude (Mbol)		4.85±0.07[2]
Details
Mass1.04[2] M☉
Radius0.99[2] R☉
Luminosity0.92[6] L☉
Surface gravity (log g)4.46[6] cgs
Temperature5,666[6] K
Metallicity [Fe/H]0.15[6] dex
Rotational velocity (v sin i)4.08[4] km/s
Age1.40[5] Gyr
Other designations
51 Ari, BD+26°503, GJ 120.2, HD 18803, HIP 14150, SAO 75696[7]
Database references
SIMBADdata
ARICNSdata

This is an ordinary G-type main sequence star with a stellar classification of G8 V.[3] Similar to the Sun, it has 1.04 times the mass and 0.99 times the Sun's radius.[2] It is 1.4[5] billion years old with a leisurely rotation rate, showing a projected rotational velocity of 4 km/s.[4] The atmospheric metallicity is higher than solar.[6] The star radiates 92%[6] of the Sun's luminosity from its photosphere at an effective temperature of 5,666 K.[6] This heat gives it the golden-hued glow of a G-type star.[9]

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. Fuhrmann, Klaus (February 2008), "Nearby stars of the Galactic disc and halo - IV", Monthly Notices of the Royal Astronomical Society, 384 (1): 173–224, 176, Bibcode:2008MNRAS.384..173F, doi:10.1111/j.1365-2966.2007.12671.x.
  3. Montes, D.; et al. (November 2001), "Late-type members of young stellar kinematic groups - I. Single stars", Monthly Notices of the Royal Astronomical Society, 328 (1): 45–63, arXiv:astro-ph/0106537, Bibcode:2001MNRAS.328...45M, doi:10.1046/j.1365-8711.2001.04781.x, S2CID 55727428.
  4. Martínez-Arnáiz, R.; et al. (September 2010), "Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter" (PDF), Astronomy and Astrophysics, 520: A79, arXiv:1002.4391, Bibcode:2010A&A...520A..79M, doi:10.1051/0004-6361/200913725, S2CID 43455849, archived from the original (PDF) on 2017-09-22, retrieved 2018-11-04.
  5. Casagrande, L.; et al. (June 2011), "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey", Astronomy and Astrophysics, 530: A138, arXiv:1103.4651, Bibcode:2011A&A...530A.138C, doi:10.1051/0004-6361/201016276, S2CID 56118016.
  6. Takeda, Yoichi (April 2007), "Fundamental Parameters and Elemental Abundances of 160 F-G-K Stars Based on OAO Spectrum Database", Publications of the Astronomical Society of Japan, 59 (2): 335–356, Bibcode:2007PASJ...59..335T, doi:10.1093/pasj/59.2.335.
  7. "LTT 10989 -- High proper-motion Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2012-08-16.
  8. van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
  9. "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, retrieved 2012-01-16
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