Astronomy:Mu Arietis

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Short description: Star system in the constellation Aries
μ Arietis
Location of μ Arietis (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Aries[1]
Right ascension  02h 42m 21.936s[2]
Declination +20° 00′ 41.28″[2]
Apparent magnitude (V) 5.74[3] (6.38/8.38/6.72/12.2)[4]
Characteristics
Spectral type A0 Vp + F2 V + A1 V[4]
U−B color index −0.03[5]
B−V color index −0.02[5]
Astrometry
Radial velocity (Rv)−6.0[6] km/s
Proper motion (μ) RA: +29.086[2] mas/yr
Dec.: −46.133[2] mas/yr
Parallax (π)7.5702 ± 0.1425[2] mas
Distance431 ± 8 ly
(132 ± 2 pc)
Absolute magnitude (MV)+0.41[1]
Orbit[7]
PrimaryAa
CompanionAb
Period (P)8.868±0.016 yr
Semi-major axis (a)0.05467±0.00067″
Eccentricity (e)0.3767±0.0087
Inclination (i)71.50±0.62°
Longitude of the node (Ω)101.07±0.75°
Periastron epoch (T)1981.133±0.089
Argument of periastron (ω)
(secondary)		96.0±3.4°
Details
μ Ari Aa
Mass3.4±1.7[8] M☉
Luminosity71.7[1] L☉
Rotational velocity (v sin i)175[9] km/s
μ Ari Ab
Mass2.1±1.7[8] M☉
Other designations
μ Ari, 34 Arietis, BD+19 403, GC 3256, HD 16811, HIP 12640, HR 793, SAO 93062, PPM 91916, WDS J02424+2001[10]
Database references
SIMBADdata

Mu Arietis is a multiple star system in the northern constellation of Aries. Its name is a Bayer designation that is Latinized from μ Arietis, and abbreviated Mu Ari or μ Ari. This system is approximately 431 light-years (132 parsecs) distant from Earth, give or take a 8 light-year margin of error, and has a combined apparent visual magnitude of 5.74.[3] According to the Bortle Dark-Sky Scale, this means it is faintly visible to the naked eye from dark suburban skies. The system is positioned near the ecliptic and is subject to lunar occultation.[8]

At the heart of this system is a close orbiting pair, designated μ Ari Aa, 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, designated μ Ari Ab, consists of a magnitude 6.72 star with a classification of A1 V, orbiting the inner pair with a period of 8.845 years and an eccentricity of 0.34.[4] The orbit of this star has been measured using lunar occultations.[8] A smaller fourth component, μ Ari B, at an angular separation of 19.1 arcseconds, has a magnitude of 12.2.[4]

According to R. H. Allen's Star Names, μ Ari together with the stars of Musca Borealis (33 Ari, 35 Ari, 39 Ari, and 41 Ari) formed the Coptic asterism Koleōn, "the Belly, or Scabbard".[11] A 1971 NASA catalog of star names listed μ Ari with the name Koleon.[12]

References

  1. ↑ 1.0 1.1 1.2 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.  XHIP record for this object at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940.  Gaia DR3 record for this source at VizieR.
  3. ↑ 3.0 3.1 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. 
  4. ↑ 4.0 4.1 4.2 4.3 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E. 
  5. ↑ 5.0 5.1 Osawa, K.; Hata, S. (1960), "Three colour photometry of B8-A2 stars.", Annals of the Tokyo Astronomical Observatory 6: 148, Bibcode: 1960AnTok...6..148O. 
  6. ↑ 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. 
  7. ↑ Mason, Brian D.; Tokovinin, Andrei; Mendez, Rene A.; Costa, Edgardo (October 2023), "Speckle Interferometry at SOAR in 2022" (in en), The Astronomical Journal 166 (4): 139, doi:10.3847/1538-3881/acedaf, ISSN 0004-6256, Bibcode: 2023AJ....166..139M .
  8. ↑ 8.0 8.1 8.2 8.3 Mason, Brian D. (1997), "Binary Star Orbits from Speckle Interferometry. XI. Orbits of Twelve Lunar Occultation Systems", The Astronomical Journal 114: 808, doi:10.1086/118514, Bibcode: 1997AJ....114..808M. 
  9. ↑ Royer, F. et al. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions", Astronomy and Astrophysics 463 (2): 671–682, doi:10.1051/0004-6361:20065224, Bibcode: 2007A&A...463..671R. 
  10. ↑ "mu. Ari". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=mu.+Ari. 
  11. ↑ Allen, R. H. (1899), Star Names: Their Lore and Meaning, p. 292, https://penelope.uchicago.edu/Thayer/E/Gazetteer/Topics/astronomy/_Texts/secondary/ALLSTA/Musca_Borealis*.html 
  12. ↑ Rhoads, Jack W. (November 15, 1971), Technical Memorandum 33-507-A Reduced Star Catalog Containing 537 Named Stars, Jet Propulsion Laboratory, California Institute of Technology, https://ntrs.nasa.gov/api/citations/19720005197/downloads/19720005197.pdf. 



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