14 Arietis

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14 Arietis
Observation data
Epoch J2000      Equinox J2000
Constellation Aries
Right ascension  02h 09m 25.3363s[1]
Declination +25° 56′ 23.612″[1]
Apparent magnitude (V) 4.98[2]
Spectral type F2 III[3]
U−B color index +0.15[2]
B−V color index +0.33[2]
Radial velocity (Rv)–1.21[4] km/s
Proper motion (μ) RA: +70.46[1] mas/yr
Dec.: -34.99[1] mas/yr
Parallax (π)11.30 ± 1.07[1] mas
Distance290 ± 30 ly
(88 ± 8 pc)
Absolute magnitude (MV)0.26[5]
Radius4[4] R
Luminosity32[4] L
Surface gravity (log g)3.2[4] cgs
Temperature6,761[4] K
Rotational velocity (v sin i)139.6[4] km/s
Other designations
BD+25°355, FK5 1089,HD 13174, HIP 10053, HR 623, SAO 75171.[6]
Database references

14 Arietis (abbreviated 14 Ari) is a star[7] in the constellation of Aries. 14 Arietis is the Flamsteed designation. It has an apparent visual magnitude of 4.98,[2] which means it is visible to the naked eye. Based upon a measured annual parallax shift of 11.30 mas,[1] is it located at a distance of approximately 290 light-years (89 parsecs), give or take a 30 light-year margin of error.

This is an astrometric binary system;[7] the primary has a stellar classification of F2 III,[3] suggesting that it is a giant star. Despite being an evolved star with four[4] times the radius of the Sun, it is spinning rapidly with a projected rotational velocity of 139.6 km/s.[4] This is causing a pronounced equatorial bulge, with the radius of the star along the equator being 24% greater than the radius at the poles;[8] the star shines at 32[4] times the luminosity of the Sun, with this energy being radiated from its outer atmosphere at an effective temperature of 6,761 K.[4] This heat gives it the yellow-white hued glow of an F-type star.[9]


  1. ^ a b c d e f 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.
  2. ^ a b c d Danziger, I. J.; Dickens, R. J. (July 1967), "Spectrophotometry of New Short-Period Variable Stars", Astrophysical Journal, 149: 55, Bibcode:1967ApJ...149...55D, doi:10.1086/149231.
  3. ^ a b Buscombe, W. (1959), "Standard stars for spectral classification", Mount Stromlo Observatory Mimeogram, 3, Bibcode:1959MtSOM...3....1B.
  4. ^ a b c d e f g h i j Massarotti, Alessandro; et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal, 135 (1): 209–231, Bibcode:2008AJ....135..209M, doi:10.1088/0004-6256/135/1/209.
  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.
  6. ^ "14 Ari". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-07-18.
  7. ^ a b 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.
  8. ^ van Belle, Gerard T. (March 2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review, 20 (1): 51, arXiv:1204.2572, Bibcode:2012A&ARv..20...51V, doi:10.1007/s00159-012-0051-2.
  9. ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on February 22, 2012, retrieved 2012-01-16

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