Astronomy:VZ Arietis

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Short description: Star in the constellation Aries
VZ Arietis
Observation data
Equinox J2000.0]] (ICRS)
Constellation Aries[1]
Right ascension  02h 48m 45.90719s[2]
Declination +25° 11′ 16.9541″[2]
Apparent magnitude (V) 5.89[1] (5.82–5.89)[3]
Characteristics
Spectral type A0 V[4]
B−V color index −0.033±0.005[1]
Variable type α2 CVn[3]
Astrometry
Radial velocity (Rv)+13.8±2.9[5] km/s
Proper motion (μ) RA: +56.600[2] mas/yr
Dec.: −0.264[2] mas/yr
Parallax (π)5.7743 ± 0.1298[2] mas
Distance560 ± 10 ly
(173 ± 4 pc)
Absolute magnitude (MV)0.48[1]
Details[6]
Mass2.74±0.09 M☉
Radius3.1[7] R☉
Luminosity78.7+15.1
−12.7 L☉
Surface gravity (log g)4.10[8] cgs
Temperature10,304+72
−71 K
Metallicity [Fe/H]+0.1[8] dex
Rotational velocity (v sin i)54 km/s
Other designations
16 Trianguli, VZ Arietis, BD+24°396, FK5 5868, HD 17471, HIP 13121, HR 830, SAO 75588[9]
Database references
SIMBADdata

VZ Arietis is single,[10] white-hued star in the northern zodiac constellation of Aries. Varying between magnitudes 5.82 and 5.89,[3] the star can be seen with the naked eye in dark, unpolluted areas. Based upon an annual parallax shift of 5.8 mas,[2] it is located 560 light-years from the Sun. It is moving further away with a heliocentric radial velocity of +14 km/s.[5] The star was formerly known as 16 Trianguli, but as the star is no longer in the constellation Triangulum, this designation has fallen out of use.[11]

In 1984, the Czechoslovak astronomer Juraj Zverko announced that the star, then called HR 830, is a variable star.[12] It was given its variable star designation, VZ Arietis, in 1987.[13]

This is a chemically peculiar star[6] of type CP2 (Ap star),[14] showing an anomalous abundance of silicon in its spectrum.[12] It has a stellar classification of A0 V,[4] which indicates this is an A-type main-sequence star that currently fusing hydrogen into helium in its core. This is an Alpha2 Canum Venaticorum variable[14] with 2.7[6] times the mass of the Sun and about 3.1[7] times the Sun's radius. It is radiating 79 times the Sun's luminosity from its photosphere at an effective temperature of 10,304 K.[6]

References

  1. ↑ 1.0 1.1 1.2 1.3 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 2.4 2.5 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. 
  3. ↑ 3.0 3.1 3.2 VSX (4 January 2010). "VZ Arietis". AAVSO Website. American Association of Variable Star Observers. http://www.aavso.org/vsx/index.php?view=detail.top&oid=3726. 
  4. ↑ 4.0 4.1 Cowley, A.; Cowley, C.; Jaschek, M.; Jaschek, C. (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. 
  5. ↑ 5.0 5.1 de Bruijne, J. H. J.; Eilers, A.-C. (October 2012). "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project". Astronomy & Astrophysics 546: 14. doi:10.1051/0004-6361/201219219. A61. Bibcode: 2012A&A...546A..61D. 
  6. ↑ 6.0 6.1 6.2 6.3 Zorec, J.; Royer, F. (2012). "Rotational velocities of A-type stars. IV. Evolution of rotational velocities". Astronomy & Astrophysics 537: A120. doi:10.1051/0004-6361/201117691. Bibcode: 2012A&A...537A.120Z. 
  7. ↑ 7.0 7.1 Pasinetti Fracassini, L. E.; Pastori, L.; Covino, S.; Pozzi, A. (2001). "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)". Astronomy & Astrophysics 367 (2): 521–24. doi:10.1051/0004-6361:20000451. Bibcode: 2001A&A...367..521P. 
  8. ↑ 8.0 8.1 Gebran, M.; Farah, W.; Paletou, F.; Monier, R.; Watson, V. (2016). "A new method for the inversion of atmospheric parameters of A/Am stars". Astronomy & Astrophysics 589: A83. doi:10.1051/0004-6361/201528052. Bibcode: 2016A&A...589A..83G. 
  9. ↑ "HD 17471". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+17471. 
  10. ↑ 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. 
  11. ↑ Wagman, M. (August 1987). "Flamsteed's Missing Stars". Journal for the History of Astronomy 18 (3): 222. doi:10.1177/002182868701800305. Bibcode: 1987JHA....18..209W. 
  12. ↑ 12.0 12.1 Zverko, J. (September 1984). "Classification of Ap-Stars HR 830 and 21 CVn". Bulletin of the Astronomical Institute of Czechoslovakia 35: 294–299. Bibcode: 1984BAICz..35..294Z. https://articles.adsabs.harvard.edu/pdf/1984BAICz..35..294Z. Retrieved 28 November 2024. 
  13. ↑ Kholopov, P. N.; Samus, N. N.; Kazarovets, E. V.; Kireeva, N. N. (August 1987). "The 68th Name-List of Variable Stars". Information Bulletin on Variable Stars 3058: 1. Bibcode: 1987IBVS.3058....1K. https://ibvs.konkoly.hu/pub/ibvs/3001/3058.pdf. Retrieved 28 November 2024. 
  14. ↑ 14.0 14.1 Wraight, K. T.; Fossati, L.; Netopil, M.; Paunzen, E.; Rode-Paunzen, M.; Bewsher, D.; Norton, A. J.; White, Glenn J. (February 2012). "A photometric study of chemically peculiar stars with the STEREO satellites - I. Magnetic chemically peculiar stars". Monthly Notices of the Royal Astronomical Society 420 (1): 757–772. doi:10.1111/j.1365-2966.2011.20090.x. Bibcode: 2012MNRAS.420..757W. 



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