Mu Arietis

The topic of Mu Arietis is an issue that has captured the interest and attention of many people around the world. Whether due to its impact on society, its historical relevance or its meaning in daily life, Mu Arietis has generated debates, investigations and even controversies. In this article, we will explore different aspects and perspectives related to Mu Arietis, with the aim of providing a broad and complete overview on this topic. From its origin to its current implications, including its influence on popular culture, we will examine in depth how Mu Arietis has left an indelible mark on history and the collective consciousness.

μ Arietis
Location of μ Arietis (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Aries
Right ascension 02h 42m 21.93980s[1]
Declination +20° 00′ 41.2612″[1]
Apparent magnitude (V) 5.74[2] (6.38/8.38/6.72/12.2)[3]
Characteristics
Spectral type A0 Vp + F2 V + A1 V[3]
U−B color index –0.03[4]
B−V color index –0.02[4]
Astrometry
Radial velocity (Rv)–6.0[5] km/s
Proper motion (μ) RA: +27.68[1] mas/yr
Dec.: –47.64[1] mas/yr
Parallax (π)9.64±0.88 mas[1]
Distance340 ± 30 ly
(104 ± 9 pc)
Absolute magnitude (MV)+0.41[6]
Orbit[7]
Period (P)8.845 ± 0.046 yr
Semi-major axis (a)0.0563 ± 0.0008″
Eccentricity (e)0.337 ± 0.023
Inclination (i)71.2 ± 1.1°
Longitude of the node (Ω)101.0 ± 1.0°
Periastron epoch (T)B 1981.099 ± 0.063
Argument of periastron (ω)
(secondary)		92.3 ± 1.7°
Details
Mass3.4 ± 1.7 (Aa) / 2.1 ± 1.7 (Ab)[7] M☉
Luminosity71.7[6] L☉
Rotational velocity (v sin i)175[8] km/s
Other designations
μ Ari, 34 Arietis, BD+19 403, HD 16811, HIP 12640, HR 793, SAO 93062.[9]
Database references
SIMBADdata

Mu Arietis, Latinized from μ Arietis, is the Bayer designation for a star system in the northern constellation of Aries. It is approximately 340 light-years (100 parsecs) distant from Earth, give or take a 30 light-year margin of error, and has a combined apparent visual magnitude of 5.74.[2] According to the Bortle Dark-Sky Scale, this means it is faintly visible to the naked eye from dark suburban skies.

At the heart of this system is a close orbiting pair consisting of a magnitude 6.38 A-type main sequence star with a stellar classification of A0 Vp and a magnitude 8.38 F-type main sequence companion with a classification of F2 V. These two components have an angular separation of 0.04 arcseconds. A third component, consisting of a magnitude 6.72 star with a classification of A1 V, is orbiting the inner pair with a period of 8.845 years and an eccentricity of 0.34. A smaller fourth component, at an angular separation of 19.1 arcseconds, has a magnitude of 12.2.[3]

References

  1. ^ a b c d e 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. ^ a b Oja, T. (August 1991). "UBV photometry of stars whose positions are accurately known. VI". Astronomy and Astrophysics Supplement Series. 89 (2): 415–419. Bibcode:1991A&AS...89..415O.
  3. ^ a b c 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.
  4. ^ a b Osawa, K.; Hata, S. (1960), "Three colour photometry of B8-A2 stars.", Annals of the Tokyo Astronomical Observatory, 6: 148, Bibcode:1960AnTok...6..148O.
  5. ^ Palmer, D. R.; et al. (1968), "The radial velocities spectral types and projected rotational velocities of 633 bright northern A stars", Royal Observatory Bulletin, 135: 385, Bibcode:1968RGOB..135..385P.
  6. ^ a b Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
  7. ^ a b Mason, Brian D. (1997). "Binary Star Orbits from Speckle Interferometry. XI. Orbits of Twelve Lunar Occultation Systems". The Astronomical Journal. 114: 808. Bibcode:1997AJ....114..808M. doi:10.1086/118514.
  8. ^ Royer, F.; Zorec, J.; Gómez, A. E. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions", Astronomy and Astrophysics, 463 (2): 671–682, arXiv:astro-ph/0610785, Bibcode:2007A&A...463..671R, doi:10.1051/0004-6361:20065224, S2CID 18475298.
  9. ^ "mu. Ari". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-08-07.{{cite web}}: CS1 maint: postscript (link)