Astronomy:40 Arietis

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Short description: Binary star in the constellation Aries
40 Arietis
Observation data
Equinox J2000.0]] (ICRS)
Constellation Aries
Right ascension  02h 48m 32.08864s[1]
Declination +18° 17′ 01.6491″[1]
Apparent magnitude (V) 5.82[2]
Characteristics
Spectral type K1 III[3]
U−B color index 1.13
B−V color index +1.20[2]
R−I color index 0.44
Variable type suspected[4]
Astrometry
Radial velocity (Rv)+47.1[5] km/s
Proper motion (μ) RA: +41.250[1] mas/yr
Dec.: −32.585[1] mas/yr
Parallax (π)7.3266 ± 0.1215[1] mas
Distance445 ± 7 ly
(136 ± 2 pc)
Absolute magnitude (MV)0.09[6]
Details[7]
Mass1.60±0.48 M☉
Radius19.74+0.29
−0.96[1] R☉
Luminosity127.98±2.52[1] L☉
Surface gravity (log g)2.09±0.11 cgs
Temperature4,473±92 K
Metallicity [Fe/H]−0.21±0.05 dex
Age2.63+1.00
−0.72 Gyr
Other designations
40 Ari, NSV 937, BD+17°442, GC 3369, HD 17459, HIP 13108, HR 828, SAO 93118[8]
Database references
SIMBADdata

40 Arietis is a probable binary star[3] system in the northern constellation of Aries. 40 Arietis is the Flamsteed designation. Their combined apparent magnitude is 5.82,[2] putting the system near the limit of naked eye visibility. Based upon an annual parallax shift of just 7.33 mas,[1] it is 445 light-years (136 parsecs) away from the Sun. At that distance, its brightness is diminished by 0.21 in magnitude from extinction caused by interstellar gas and dust.[9]

This is a suspected spectroscopic binary with an angular separation of 0.2″ between the two components.[3] The visible component is an evolved giant star with a stellar classification of K1 III.[3] It is a suspected variable star of unknown type,[4] and is around 2.6 billion years old with 1.6 times the mass of the Sun.[7] With the supply of hydrogen at its core exhausted, the star has expanded to 20 times the Sun's radius.[1] It is radiating 128 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,473 K.[7]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 Nicolet, B. (1978), "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System", Astronomy and Astrophysics Supplement Series 34: 1–49, Bibcode: 1978A&AS...34....1N. 
  3. ↑ 3.0 3.1 3.2 3.3 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. 
  4. ↑ 4.0 4.1 Samus, N. N. et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1 61 (1): 80–88, doi:10.1134/S1063772917010085, Bibcode: 2017ARep...61...80S. 
  5. ↑ Wilson, Ralph Elmer (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication (Washington: Carnegie Institution of Washington), Bibcode: 1953GCRV..C......0W. 
  6. ↑ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  7. ↑ 7.0 7.1 7.2 Feuillet, Diane K. et al. (2016), "Determining Ages of APOGEE Giants with Known Distances", The Astrophysical Journal 817 (1): 40, doi:10.3847/0004-637X/817/1/40, Bibcode: 2016ApJ...817...40F. 
  8. ↑ "40 Ari". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=40+Ari. 
  9. ↑ Famaey, B. et al. (January 2005), "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters", Astronomy and Astrophysics 430 (1): 165–186, doi:10.1051/0004-6361:20041272, Bibcode: 2005A&A...430..165F. 



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