Mu Arietis
Today, Mu Arietis is one of the most relevant and discussed topics in various areas. Its impact is reflected in society, the economy, politics and culture. With the advancement of technology and globalization, Mu Arietis has gained greater importance and has generated endless debates and research. From different perspectives, we seek to understand and analyze its influence in today's world. Given this scenario, it is essential to explore the multiple dimensions that Mu Arietis encompasses, as well as its implications at a global and local level. In this article, we will delve into the fascinating universe of Mu Arietis, to understand its complexity and its relevance today.
  | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| 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 mas/yr[2] Dec.: −46.133 mas/yr[2] |
| Parallax (π) | 7.5702±0.1425 mas[2] |
| Distance | 431 ± 8 ly (132 ± 2 pc) |
| Absolute magnitude (MV) | +0.41[1] |
| 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 | |
| μ Ari Aa | |
| Mass | 3.4±1.7[7] M☉ |
| Luminosity | 71.7[1] L☉ |
| Rotational velocity (v sin i) | 175[8] km/s |
| μ Ari Ab | |
| Mass | 2.1±1.7[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[9] | |
| 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.[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.[7]
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.[7] A smaller fourth component, μ Ari B, at an angular separation of 19.1 arcseconds, has a magnitude of 12.2.[4]
References
- ^ a b c 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.
- ^ a b c d 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.
- ^ 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.
- ^ a b c d 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.
- ^ 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.
- ^ 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.
- ^ a b c d e 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.
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