52 Arietis

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52 Arietis
Observation data
Epoch J2000      Equinox J2000
Constellation Aries
Right ascension  03h 05m 26.68819s[1]
Declination +25° 15′ 18.6257″[1]
Apparent magnitude (V) 5.46[2]
Spectral type B7 V + B7 V[3]
U−B color index -0.38[2]
B−V color index -0.03[2]
Radial velocity (Rv)9[4] km/s
Proper motion (μ) RA: +1.44[1] mas/yr
Dec.: -10.26[1] mas/yr
Parallax (π)6.05 ± 1.06[1] mas
Distanceapprox. 540 ly
(approx. 170 pc)
Primary52 Ari A
Companion52 Ari B
Period (P)227[5] yr
Semi-major axis (a)0.47″
Eccentricity (e)0.73[5]
Inclination (i)77.5°
Longitude of the node (Ω)92.8°
Periastron epoch (T)1938.5
52 Ari A
Mass5.12[6] M
Radius3.3[7] R
Luminosity452[8] L
Temperature12,912[8] K
Rotational velocity (v sin i)159[8] km/s
52 Ari B
Mass5.12[6] M
Other designations
52 Arietis, ADS 2336, BD+24° 431, HIP 14376.[3]
52 Ari A: HD 19134, HR 927.
52 Ari B: HD 19135, HR 928.
Database references
52 Ari A
52 Ari B

52 Arietis (abbreviated 52 Ari) is a triple star system in the northern constellation of Aries. 52 Arietis is the Flamsteed designation. The combined apparent magnitude is +5.46,[2] which is bright enough to be faintly visible to the naked eye. Based upon an annual parallax shift of 6.05 mas,[1] the system is roughly 540 light-years (170 parsecs) distant from the Earth. The inner pair of this system consist of two nearly identical B-type main sequence stars, each with about five times the mass of the Sun. The tertiary component is a smaller star with 88% of the Sun's mass, and is a common proper motion companion.[6]


  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 Eggen, Olin J. (1966), "Three-colour photometry of the components in wide double and multiple systems II", Royal Observatory bulletins. Series E (120): 333–403, Bibcode:1966RGOB..120..333E
  3. ^ a b "52 Ari". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-08-16.
  4. ^ Wilson, Ralph Elmer (1953). General Catalogue of Stellar Radial Velocities. Washington: Carnegie Institution of Washington. Bibcode:1953GCRV..C......0W.
  5. ^ a b Abt, Helmut A. (August 2005), "Observed Orbital Eccentricities", The Astrophysical Journal, 629 (1): 507–511, Bibcode:2005ApJ...629..507A, doi:10.1086/431207.
  6. ^ a b c Tokovinin, A. (September 2008), "Comparative statistics and origin of triple and quadruple stars", Monthly Notices of the Royal Astronomical Society, 389 (2): 925–938, arXiv:0806.3263, Bibcode:2008MNRAS.389..925T, doi:10.1111/j.1365-2966.2008.13613.x.
  7. ^ Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics", Astronomy and Astrophysics, 367: 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451.
  8. ^ a b c Zorec, J.; Royer, F. (January 2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691.

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