63 Andromedae
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Andromeda |
| Right ascension | 02h 20m 58.21s[1] |
| Declination | +50° 09′ 05.3″[1] |
| Apparent magnitude (V) | 5.59[2] |
| Characteristics | |
| Spectral type | B9VpSi[3] |
| B−V color index | –0.089[1] |
| Variable type | α² CVn[2] |
| Astrometry | |
| Radial velocity (Rv) | –0.30[4] km/s |
| Proper motion (μ) | RA: 39.389±0.243[5] mas/yr Dec.: −31.197±0.210[5] mas/yr |
| Parallax (π) | 7.8991 ± 0.1090[5] mas |
| Distance | 413 ± 6 ly (127 ± 2 pc) |
| Absolute magnitude (MV) | +0.26[6] |
| Details[6] | |
| Mass | 3.07 ± 0.14 M☉ |
| Radius | 2.4 ± 0.3 R☉ |
| Luminosity | 110 L☉ |
| Surface gravity (log g) | 4.29 ± 0.11 cgs |
| Temperature | 11,967 K |
| Rotation | 4.189 days |
| Other designations | |
| Database references | |
| SIMBAD | data |
63 Andromedae (abbreviated 63 And) is an Alpha2 Canum Venaticorum (α2 CVn) variable star in the constellation Andromeda. Its variable star designation is PZ Andromedae. With an apparent magnitude of about 5.6, it's bright enough to be seen by naked eye. Based upon an annual parallax shift of 7.8991 mas, it is located 413 light years away.
The spectral type of this star is B9VpSi, indicating that it's a chemically peculiar main sequence star with abnormally strong silicon lines. Although it has a B-type spectral class, this type of star is known as an Ap star, a class of stars with very strong spectral lines of certain heavy elements and strong magnetic fields. The chemical peculiarities are caused by stratification in the atmosphere due to slow rotation.[7]
The star has 3 times the mass of the Sun and 2.4 times the Sun's radius. It is radiating 110 times the Sun's luminosity from its photosphere at an effective temperature of 11,967 K.[6]
63 Andromedae varies in brightness by about 0.05 magnitudes with a period of 4.189 days. This is believed to occur as it rotates. This type of variable star is known as an α2 Canum Venaticorum varibale after the first example to be studied.[2]
References
- 1 2 3 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. Vizier catalog entry
- 1 2 3 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/gcvs. Originally Published In: 2009yCat....102025S. 1: B/gcvs. Bibcode:2009yCat....102025S.
- ↑ Abt, H. A.; Morrell, N. I. (July 1995), "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars", Astrophysical Journal Supplement, 99: 135, Bibcode:1995ApJS...99..135A, doi:10.1086/192182.
- ↑ 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, A61.
- 1 2 3 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. Gaia DR2 record for this source at VizieR.
- 1 2 3 North, P. (June 1998), "Do SI stars undergo any rotational braking?", Astronomy and Astrophysics, 334: 181–187, arXiv:astro-ph/9802286, Bibcode:1998A&A...334..181N
- ↑ Renson, P.; Manfroid, J. (2009). "Catalogue of Ap, HgMn and Am stars". Astronomy and Astrophysics. 498 (3): 961. Bibcode:2009A&A...498..961R. doi:10.1051/0004-6361/200810788.