Astronomy:V Cephei
From HandWiki
Short description: Star in the constellation Cepheus
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Cepheus |
| Right ascension | 23h 56m 27.804s[1] |
| Declination | +83° 11′ 28.02″[1] |
| Apparent magnitude (V) | 6.57[2] |
| Characteristics | |
| Spectral type | A1V[3] |
| B−V color index | +0.07[2] |
| Astrometry | |
| Radial velocity (Rv) | −18.74[1] km/s |
| Proper motion (μ) | RA: +50.676[1] mas/yr Dec.: +6.869[1] mas/yr |
| Parallax (π) | 11.1865 ± 0.0264[1] mas |
| Distance | 291.6 ± 0.7 ly (89.4 ± 0.2 pc) |
| Absolute magnitude (MV) | +1.78[4] |
| Details | |
| Mass | 2.27[5] M☉ |
| Radius | 1.7[5] R☉ |
| Luminosity | 17.4[5] L☉ |
| Surface gravity (log g) | 4.33[5] cgs |
| Temperature | 9,004[5] K |
| Metallicity [Fe/H] | −0.25[6] dex |
| Rotational velocity (v sin i) | 147[7] km/s |
| Age | 373[7] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
V Cephei is a white main sequence star in the constellation Cepheus. It only varies slightly by 0.03 of a magnitude. It was suspected of being variable by American astronomer Seth Carlo Chandler noting in 1890 that it varied by 0.7 magnitude but that it needed more confirmation. Subsequent observers were divided in whether they noted variability or not.[9] A subsequent study with photoelectric photometry showed no variability.[10]
With a spectral class of A1V, V Cephei is a main sequence star with a surface temperature of 9,004 K. It has twice the mass of the Sun and, with nearly twice its radius, it shines at 17 L☉.
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 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.
- ↑ 2.0 2.1 Oja, T. (August 1991). "UBV photometry of stars whose positions are accurately known. VI.". Astronomy and Astrophysics Supplement Series 89: 415. ISSN 0365-0138. Bibcode: 1991A&AS...89..415O.
- ↑ 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.
- ↑ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.
- ↑ 5.0 5.1 5.2 5.3 5.4 Stassun, Keivan G. et al. (2019-10-01). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal 158 (4): 138. doi:10.3847/1538-3881/ab3467. ISSN 0004-6256. Bibcode: 2019AJ....158..138S.
- ↑ Anders, F.; Khalatyan, A.; Chiappini, C.; Queiroz, A. B.; Santiago, B. X.; Jordi, C.; Girardi, L.; Brown, A. G. A. et al. (2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy and Astrophysics 628: A94. doi:10.1051/0004-6361/201935765. Bibcode: 2019A&A...628A..94A.
- ↑ 7.0 7.1 David, Trevor J.; Hillenbrand, Lynne A. (2015). "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets". The Astrophysical Journal 804 (2): 146. doi:10.1088/0004-637X/804/2/146. Bibcode: 2015ApJ...804..146D.
- ↑ "V* V Cep". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V%2A+V+Cep.
- ↑ Hoffleit, Dorrit (1985). "Was Harlow Shapley Right About V Cephei?". The Journal of the American Association of Variable Star Observers 14 (2): 64–66. Bibcode: 1985JAVSO..14...64H.
- ↑ Fortier, George (1989). "Photoelectric Photometry of V Cephei". The Journal of the American Association of Variable Star Observers 18 (1): 49–51. Bibcode: 1989JAVSO..18...49F.
 |  |
