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31 Arietis

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Binary star system in the constellation Aries
31 Arietis
Observation data
Epoch J2000      Equinox J2000
Constellation Aries
Right ascension 02 36 37.91730
Declination +12° 26′ 51.4867″
Apparent magnitude (V) 5.75 (5.68 + 5.78)
Characteristics
Spectral type F7 V + F7 V
U−B color index –0.05
B−V color index +0.47
Astrometry
Radial velocity (Rv)+8.8 km/s
Proper motion (μ) RA: +282.19 mas/yr
Dec.: –86.84 mas/yr
Parallax (π)28.79 ± 0.43 mas
Distance113 ± 2 ly
(34.7 ± 0.5 pc)
Absolute magnitude (MV)2.94
Orbit
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 K
Metallicity –0.25 dex
Rotational velocity (v sin i)5 km/s
Age2.8 Gyr
Other designations
BD+11 360, FK5 2179, HD 16234, HIP 12153, HR 763, SAO 93022, WDS J02366+1227.
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. The pair have an apparent visual magnitude of 5.75, which is just bright enough to be faintly visible to the naked eye. Based upon an annual parallax shift of 28.79 mas, 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. The dynamical mass of the system is 3.36 ± 0.04 M.

References

  1. ^ 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. ^ 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. ^ 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. ^ "31 Ari". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-08-14.
  5. ^ 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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