 Three light curves for V803 Centauri, on three timescales, hours (plot A), days (plot B) and years (plot C). Adapted from Patterson et al. (2000),[1] Kato et al. (2004)[2] and Levitan et al. (2015)[3] | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Centaurus |
| Right ascension | 13h 23m 44.54s[4] |
| Declination | −41° 44′ 29.54″[4] |
| Apparent magnitude (V) | 13.2[5] (var) |
| Characteristics | |
| Spectral type | pec |
| U−B color index | -0.9 - -1.0[6] |
| B−V color index | 0.0.1[6] |
| Variable type | AM CVn[7] |
| Astrometry | |
| Proper motion (μ) | RA: -3.907[4] mas/yr Dec.: +11.978[4] mas/yr |
| Parallax (π) | 3.4885 ± 0.0599 mas[4] |
| Distance | 930 ± 20 ly (287 ± 5 pc) |
| Absolute magnitude (MV) | 5.93[7] |
| Details | |
| White dwarf | |
| Mass | 0.9-1.2[7] M☉ |
| Donor star | |
| Mass | 0.06-0.11[7] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
V803 Centauri (V803 Cen) is a cataclysmic binary consisting of a dwarf helium star losing mass to a white dwarf. It is an example of the AM Canum Venaticorum (AM CVn) type of cataclysmic variable stars.[1]
References
- ^ a b Patterson, Joseph; Walker, Stan; Kemp, Jonathan; O'Donoghue, Darragh; Bos, Marc; Stubbings, Rod (2000). "V803 Centauri: A Helium‐rich Dwarf Nova". Publications of the Astronomical Society of the Pacific. The University of Chicago Press on behalf of the Astronomical Society of the Pacific. 112 (771): 625–631. Bibcode:2000PASP..112..625P. doi:10.1086/316561. JSTOR 316561.
- ^ Kato, Taichi; Stubbings, Rod; Monard, Berto; Butterworth, Neil D.; Bolt, Greg; Richards, Tom (March 25, 2004). "V803 Centauri: Helium Dwarf Nova Mimicking a WZ Sge-Type Superoutburst". Publications of the Astronomical Society of Japan. 56: S89–S98. arXiv:astro-ph/0307308. Bibcode:2004PASJ...56S..89K. doi:10.1093/pasj/56.sp1.S89.
- ^ Levitan, David; Groot, Paul J.; Prince, Thomas A.; Kulkarni, Shrinivas R.; Laher, Russ; Ofek, Eran O.; Sesar, Branimir; Surace, Jason (January 2015). "Long-term photometric behaviour of outbursting AM CVn systems". Monthly Notices of the Royal Astronomical Society. 446 (1): 391–410. arXiv:1410.6987. Bibcode:2015MNRAS.446..391L. doi:10.1093/mnras/stu2105.
- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ Samus', N. N.; Goranskii, V. P.; Durlevich, O. V.; Zharova, A. V.; Kazarovets, E. V.; Kireeva, N. N.; Pastukhova, E. N.; Williams, D. B.; Hazen, M. L. (2003). "An Electronic Version of the Second Volume of the General Catalogue of Variable Stars with Improved Coordinates". Astronomy Letters. 29 (7): 468. Bibcode:2003AstL...29..468S. doi:10.1134/1.1589864. S2CID 16299532.
- ^ a b Elvius, A. (1975). "Variable blue object with a peculiar spectrum". Astronomy and Astrophysics. 44: 117. Bibcode:1975A&A....44..117E.
- ^ a b c d Solheim, J.-E. (2010). "AM CVn Stars: Status and Challenges". Publications of the Astronomical Society of the Pacific. 122 (896): 1133–1163. Bibcode:2010PASP..122.1133S. doi:10.1086/656680.
 | This variable star–related article is a stub. You can help Wikipedia by expanding it. |
 | This article about a white dwarf is a stub. You can help Wikipedia by expanding it. |
This page was last edited on 20 September 2023, at 04:59