Astronomy:49 Arietis

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Short description: Star in the constellation Aries
49 Arietis
Observation data
Equinox J2000.0]] (ICRS)
Constellation Aries
Right ascension  03h 01m 54.14125s[1]
Declination +26° 27′ 44.4746″[1]
Apparent magnitude (V) 5.90[2]
Characteristics
Evolutionary stage main sequence[1]
Spectral type kA2hA6mA7[3]
U−B color index +0.12[2]
B−V color index +0.141±0.006[4]
Astrometry
Radial velocity (Rv)−1.0[5] km/s
Proper motion (μ) RA: −14.323[1] mas/yr
Dec.: +5.160[1] mas/yr
Parallax (π)14.6587 ± 0.0844[1] mas
Distance223 ± 1 ly
(68.2 ± 0.4 pc)
Absolute magnitude (MV)1.87[4]
Details
Mass1.9[1] M☉
Radius2.0[1] R☉
Luminosity16.1[1] L☉
Surface gravity (log g)4.34[6] cgs
Temperature8,424[6] K
Metallicity [Fe/H]−0.02[6] dex
Rotational velocity (v sin i)52[5] km/s
Age704[1] Myr
Other designations
49 Ari, NSV 1021, BD+25°477, HD 18769, HIP 14109, HR 905, SAO 75693[7]
Database references
SIMBADdata

49 Arietis is a single[8] star in the northern constellation of Aries. 49 Arietis is the Flamsteed designation. It is visible to the naked eye as a faint, white hued star with an apparent visual magnitude of 5.90.[2] The star is located at a distance of about 223 light-years (68 parsecs) distant from Earth based on parallax.

This object is classified as an Am star,[9] or non-magnetic chemically peculiar star of the CP1[10] class, which means the spectrum displays abnormal abundances of certain heavier elements. It has a stellar classification of kA2hA6mA7, which means it has the calcium K line of an A2 class star, the hydrogen lines of an A6 star, and the metal lines of an A7 star. 49 Arietis has a moderately high rate of spin, showing a projected rotational velocity of 52 km/s, and is radiating 16 times the luminosity of the Sun from its photosphere at an effective temperature of 8,424 K.

References

  1. ↑ 1.00 1.01 1.02 1.03 1.04 1.05 1.06 1.07 1.08 1.09 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.
  2. ↑ 2.0 2.1 2.2 Oja, T. (April 1983), "UBV photometry of FK4 and FK4 supplement stars", Astronomy and Astrophysics Supplement Series 52: 131–134, Bibcode: 1983A&AS...52..131O. 
  3. ↑ Abt, Helmut A.; Morrell, Nidia I. (1995), "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars", Astrophysical Journal Supplement 99: 135, doi:10.1086/192182, Bibcode: 1995ApJS...99..135A. 
  4. ↑ 4.0 4.1 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  5. ↑ 5.0 5.1 Wielen, R. et al. (1999), "Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic fundamental stars with direct solutions", Veroeffentlichungen des Astronomischen Rechen-Instituts Heidelberg (Astronomisches Rechen-Institut Heidelberg) 35 (35): 1, Bibcode: 1999VeARI..35....1W. 
  6. ↑ 6.0 6.1 6.2 Koleva, M.; Vazdekis, A. (February 2012), "Stellar population models in the UV. I. Characterisation of the New Generation Stellar Library", Astronomy & Astrophysics 538: A143, doi:10.1051/0004-6361/201118065, Bibcode: 2012A&A...538A.143K. 
  7. ↑ "49 Ari". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=49+Ari. 
  8. ↑ Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society 389 (2): 869, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E. 
  9. ↑ Cowley, A. et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal 74: 375–406, doi:10.1086/110819, Bibcode: 1969AJ.....74..375C. 
  10. ↑ Paunzen, E. et al. (February 2013), "A photometric study of chemically peculiar stars with the STEREO satellites - II. Non-magnetic chemically peculiar stars", Monthly Notices of the Royal Astronomical Society 429 (1): 119–125, doi:10.1093/mnras/sts318, Bibcode: 2013MNRAS.429..119P. 



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