31 Arietis
Observation data
Epoch J2000      Equinox J2000
Constellation Aries
Right ascension 02h 36m 37.91730s[1]
Declination +12° 26′ 51.4867″[1]
Apparent magnitude (V) 5.75[2] (5.68 + 5.78)[3]
Characteristics
Spectral type F7 V + F7 V[3]
U−B color index –0.05[4]
B−V color index +0.47[4]
Astrometry
Radial velocity (Rv)+8.8 km/s
Proper motion (μ) RA: +282.19[1] mas/yr
Dec.: –86.84[1] mas/yr
Parallax (π)28.79 ± 0.43 mas[1]
Distance113 ± 2 ly
(34.7 ± 0.5 pc)
Absolute magnitude (MV)2.94[5]
Orbit[3]
Period (P)3.80 ± 0.10 yr
Semi-major axis (a)0.077 ± 0.001″
Eccentricity (e)0.017 ± 0.002
Inclination (i)112.7 ± 0.5°
Longitude of the node (Ω)145.0 ± 0.5°
Periastron epoch (T)2010.28 ± 0.15
Argument of periastron (ω)
(secondary)		3.7 ± 15.0°
Details
Temperature6,137[5] K
Metallicity [Fe/H]–0.25[5] dex
Rotational velocity (v sin i)5[6] km/s
Age2.8[5] Gyr
Other designations
BD+11 360, FK5 2179, HD 16234, HIP 12153, HR 763, SAO 93022, WDS J02366+1227.[4]
Database references
SIMBADdata

31 Arietis (abbreviated 31 Ari) is a binary star in the northern constellation of Aries. 31 Arietis is the Flamsteed designation. The two members of this system orbit each other with a period of 3.80 years and an eccentricity of 0.017. Both components of the system are F-type main sequence stars with a stellar classification of F7 V.[3] The pair have an apparent visual magnitude of 5.75,[2] which is just bright enough to be faintly visible to the naked eye. Based upon an annual parallax shift of 28.79 mas,[1] the distance to this system is approximately 113 light-years (35 parsecs). The system is located near the ecliptic, so it is subject to occultation by the Moon.[7] The dynamical mass of the system is 3.36 ± 0.04 M☉.[3]

References

  1. 1 2 3 4 5 6 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.
  2. 1 2 Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  3. 1 2 3 4 5 Docobo, J. A.; Tamazian, V. S.; Malkov, O. Yu.; Campo, P. P.; Chulkov, D. A. (June 2016). "Improved orbits and parallaxes for eight visual binaries with unrealistic previous masses using the Hipparcos parallax". Monthly Notices of the Royal Astronomical Society. 459 (2): 1580–1585. arXiv:1609.03392. Bibcode:2016MNRAS.459.1580D. doi:10.1093/mnras/stw709.
  4. 1 2 3 "31 Ari". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-08-14.
  5. 1 2 3 4 Holmberg, J.; Nordström, B.; Andersen, J. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv:0811.3982, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191, S2CID 118577511.
  6. ↑ Bernacca, P. L.; Perinotto, M. (1970), "A catalogue of stellar rotational velocities", Contributi Osservatorio Astronomico di Padova in Asiago, 239 (1): 1, Bibcode:1970CoAsi.239....1B.
  7. ↑ Richichi, A.; et al. (January 2016), "Lunar Occultations of 18 Stellar Sources from the 2.4 m Thai National Telescope", The Astronomical Journal, 151 (1): 5, Bibcode:2016AJ....151...10R, doi:10.3847/0004-6256/151/1/10, S2CID 119258140, 10.


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