VZ Arietis
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Aries |
| Right ascension | 02h 48m 45.90719s[1] |
| Declination | +25° 11′ 16.95410″[1] |
| Apparent magnitude (V) | 5.89[2] (5.82 - 5.89)[3] |
| Characteristics | |
| Spectral type | A0 V[4] |
| B−V color index | −0.033±0.005[2] |
| Variable type | α2 CVn[3] |
| Astrometry | |
| Radial velocity (Rv) | +13.8±2.9[5] km/s |
| Proper motion (μ) | RA: +56.600[1] mas/yr Dec.: −0.264[1] mas/yr |
| Parallax (π) | 5.7743 ± 0.1298 mas[1] |
| Distance | 560 ± 10 ly (173 ± 4 pc) |
| Absolute magnitude (MV) | 0.48[2] |
| Details[6] | |
| Mass | 2.74±0.09 M☉ |
| Radius | 3.1[7] R☉ |
| Luminosity | 78.7+15.1 −12.7 L☉ |
| Surface gravity (log g) | 4.10[8] cgs |
| Temperature | 10,304+72 −71 K |
| Metallicity [Fe/H] | +0.1[8] dex |
| Rotational velocity (v sin i) | 54 km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
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,[1] 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 Czechoslovakian 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
[edit]- ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051.
- ^ 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. S2CID 119257644.
- ^ a b c VSX (4 January 2010). "VZ Arietis". AAVSO Website. American Association of Variable Star Observers. Retrieved 15 June 2014.
- ^ a b Cowley, A.; et al. (April 1969). "A study of the bright A stars. I. A catalogue of spectral classifications". Astronomical Journal. 74: 375–406. Bibcode:1969AJ.....74..375C. doi:10.1086/110819.
- ^ a b 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. arXiv:1208.3048. Bibcode:2012A&A...546A..61D. doi:10.1051/0004-6361/201219219. S2CID 59451347. A61.
- ^ a b c d Zorec, J.; Royer, F. (2012). "Rotational velocities of A-type stars. IV. Evolution of rotational velocities". Astronomy & Astrophysics. 537: A120. arXiv:1201.2052. Bibcode:2012A&A...537A.120Z. doi:10.1051/0004-6361/201117691. S2CID 55586789.
- ^ a b Pasinetti Fracassini, L. E.; et al. (2001). "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)". Astronomy & Astrophysics. 367 (2) (Third ed.): 521–24. arXiv:astro-ph/0012289. Bibcode:2001A&A...367..521P. doi:10.1051/0004-6361:20000451. S2CID 425754.
- ^ a b Gebran, M.; et al. (2016). "A new method for the inversion of atmospheric parameters of A/Am stars". Astronomy & Astrophysics. 589: A83. arXiv:1603.01146. Bibcode:2016A&A...589A..83G. doi:10.1051/0004-6361/201528052. S2CID 118549566.
- ^ "HD 17471". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 22 August 2018.
- ^ 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.
- ^ Wagman, M. (August 1987). "Flamsteed's Missing Stars". Journal for the History of Astronomy. 18 (3): 222. Bibcode:1987JHA....18..209W. doi:10.1177/002182868701800305. S2CID 118445625.
- ^ a b 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. Retrieved 28 November 2024.
- ^ Kholopov, P. N.; Samus, N. N.; Kazarovets, E. V.; Kireeva, N. N. (August 1987). "The 68th Name-List of Variable Stars" (PDF). Information Bulletin on Variable Stars. 3058. Bibcode:1987IBVS.3058....1K. Retrieved 28 November 2024.
- ^ a b Wraight, K. T.; et al. (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. arXiv:1110.6283. Bibcode:2012MNRAS.420..757W. doi:10.1111/j.1365-2966.2011.20090.x. S2CID 14811051.
