Mu Arietis
  | |
| Observation data Epoch J2000 Equinox ICRS | |
|---|---|
| Constellation | Aries |
| Right ascension | 02h 42m 21.936s |
| Declination | +20° 00′ 41.28″ |
| Apparent magnitude (V) | 5.74 (6.38/8.38/6.72/12.2) |
| Characteristics | |
| Spectral type | A0 Vp + F2 V + A1 V |
| U−B color index | −0.03 |
| B−V color index | −0.02 |
| Astrometry | |
| Radial velocity (Rv) | −6.0 km/s |
| Proper motion (μ) | RA: +29.086 mas/yr Dec.: −46.133 mas/yr |
| Parallax (π) | 7.5702±0.1425 mas |
| Distance | 431 ± 8 ly (132 ± 2 pc) |
| Absolute magnitude (MV) | +0.41 |
| Orbit | |
| Primary | Aa |
| Secondary | Ab |
| 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 | |
| Mass | 3.4±1.7 M☉ |
| Luminosity | 71.7 L☉ |
| Rotational velocity (v sin i) | 175 km/s |
| μ Ari Ab | |
| Mass | 2.1±1.7 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 | |
| Database references | |
| SIMBAD | data |
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. 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.
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. The orbit of this star has been measured using lunar occultations. A smaller fourth component, μ Ari B, at an angular separation of 19.1 arcseconds, has a magnitude of 12.2.
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". A 1971 NASA catalog of star names listed μ Ari with the name Koleon.
References
- 1 2 3 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. XHIP record for this object at VizieR.
- 1 2 3 4 5 Vallenari, A.; et al. (Gaia collaboration) (2023), "Gaia Data Release 3. Summary of the content and survey properties", Astronomy and Astrophysics, 674: A1, arXiv:2208.00211, Bibcode:2023A&A...674A...1G, doi:10.1051/0004-6361/202243940, S2CID 244398875. Gaia DR3 record for this source at VizieR.
- 1 2 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.
- 1 2 3 4 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.
- 1 2 Osawa, K.; Hata, S. (1960), "Three colour photometry of B8-A2 stars.", Annals of the Tokyo Astronomical Observatory, 6: 148, Bibcode:1960AnTok...6..148O.
- ↑ 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.
- ↑ Mason, Brian D.; Tokovinin, Andrei; Mendez, Rene A.; Costa, Edgardo (October 2023), "Speckle Interferometry at SOAR in 2022", The Astronomical Journal, 166 (4): 139, Bibcode:2023AJ....166..139M, doi:10.3847/1538-3881/acedaf, ISSN 0004-6256.
- 1 2 3 4 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.
- ↑ Royer, F.; et al. (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.
- ↑ "mu. Ari". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-08-07.
{{cite web}}: CS1 maint: postscript (link) - ↑ Allen, R. H. (1899), Star Names: Their Lore and Meaning, p. 292
- ↑ Rhoads, Jack W. (November 15, 1971), Technical Memorandum 33-507-A Reduced Star Catalog Containing 537 Named Stars (PDF), Jet Propulsion Laboratory, California Institute of Technology.
