BV Centauri
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Centaurus |
| Right ascension | 13h 31m 19.485s[2] |
| Declination | −54° 58′ 33.52″[2] |
| Apparent magnitude (V) | 13.05[3] (10.7 to 14.0)[4] |
| Characteristics | |
| Spectral type | G5-G8IV-V (secondary)[3] |
| U−B color index | -0.22[3] |
| B−V color index | 0.77[3] |
| Variable type | SS Cyg[4] |
| Astrometry | |
| Radial velocity (Rv) | -22.3[5] km/s |
| Proper motion (μ) | RA: -25.8[2] mas/yr Dec.: -1.4[2] mas/yr |
| Parallax (π) | 2.81 ± 0.38 mas[6] |
| Distance | approx. 1,200 ly (approx. 360 pc) |
| Absolute magnitude (MV) | +3.0 - +5.8[6] |
| Orbit | |
| Period (P) | 0.611±0.002 days[5] |
| Semi-major axis (a) | 2.53×1011 cm (0.017 au)[7] |
| Inclination (i) | 53±4,[5] 62±5[7]° |
| Semi-amplitude (K1) (primary) | 128±3[7] km/s |
| Semi-amplitude (K2) (secondary) | 137.3±0.3[5] km/s |
| Details | |
| Primary (white dwarf) | |
| Mass | 1.18+0.28 −0.16[5] M☉ |
| Surface gravity (log g) | 8.3[8] cgs |
| Temperature | 40000 ± 1000[8] K |
| Rotational velocity (v sin i) | 500 ± 100[8] km/s |
| Secondary | |
| Mass | 1.05+0.23 −0.14[5] M☉ |
| Radius | 1.41 ± 0.04[7] R☉ |
| Surface gravity (log g) | 3.5[5] cgs |
| Temperature | 5250[5] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
BV Centauri is a cataclysmic variable binary star in the constellation Centaurus. It is a dwarf nova, and undergoes rapid increases in brightness that are recurrent with a mean period of 150 days. This period seems to have increased in the last few decades.[10] During quiescence, its visual apparent magnitude is about 13, with variations of a few tenths of magnitude over an orbit due to differences in the star's visible surface area (ellipsoidal variability),[7] brightening to a maximum magnitude of 10.7 during outbursts.[4] From its luminosity, it is estimated that the system is about 500 parsecs (1,600 ly) away from Earth.[3][7] A Gaia parallax of 2.81 mas has been measured, corresponding to about 360 pc.[6]
Cataclysmic variables are short-period binary systems in which a white dwarf primary accretes matter from a secondary star. For BV Centauri, the white dwarf and its companion have estimated masses of 1.18 and 1.05 times the mass of the Sun respectively,[5] although alternate, conflicting mass measurements were reported too.[11] The secondary is a conventional star with a spectral type of G5-G8IV-V and it is assumed to contribute to half of the visual luminosity of the system. It is thought to have a radius of 1.4 R☉ and so to be significantly evolved away from the zero age main sequence.[3][7] The reconstruction of its surface by Doppler imaging revealed it to be a highly magnetically active star, with about 25% of its surface covered in starspots which are much more abundant on the hemisphere facing the white dwarf. Furthermore, a prominence was detected above the secondary star's surface, also in the side facing the white dwarf.[5] The white dwarf primary can be observed clearly at ultraviolet wavelengths where it is the strongest source. Any accretion disk in the system appears relatively faint.[8]
The system has a period of 0.611179 days (16.7 hours), one of the longest periods for a dwarf nova, and is inclined by 53 ± 4° in relation to the plane of the sky.[5]
It has been noted that BV Centauri's light curve during outbursts has anomalous behavior for a dwarf nova, with a long interval of up to 15 days before reaching peak brightness and no plateau at maximum brightness, and it has been compared to the classic nova GK Persei. Based on this, it has been proposed that BV Centauri could have generated an unobserved nova outburst in the 19th century, which was missed by the observers at the time.[10][12]
References
[edit]- ^ Kiraga, M. (March 2012). "ASAS Photometry of ROSAT Sources. I. Periodic Variable Stars Coincident with Bright Sources from the ROSAT All Sky Survey". Acta Astronomica. 62 (1): 67–95. arXiv:1204.3825. Bibcode:2012AcA....62...67K. Retrieved 28 November 2021.
- ^ a b c d Høg, E; Fabricius, C; Makarov, V. V; Urban, S; Corbin, T; Wycoff, G; Bastian, U; Schwekendiek, P; Wicenec, A (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27. Bibcode:2000A&A...355L..27H.
- ^ a b c d e f Vogt, N; Breysacher, J (February 1980). "The dwarf nova BV Centauri - A spectroscopic binary". Astrophysical Journal. 235: 945–954. Bibcode:1980ApJ...235..945V. doi:10.1086/157699.
- ^ a b c Samus, N. N; Durlevich, O. V; et al. (January 2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/gcvs. 1. Bibcode:2009yCat....102025S. VizieR table entry
- ^ a b c d e f g h i j k Watson, C. A; Steeghs, D; Shahbaz, T; Dhillon, V. S (December 2007). "Roche tomography of cataclysmic variables - IV. Star-spots and slingshot prominences on BV Cen". Monthly Notices of the Royal Astronomical Society. 382 (3): 1105–1118. arXiv:0707.0739. Bibcode:2007MNRAS.382.1105W. doi:10.1111/j.1365-2966.2007.12173.x. S2CID 2073273.
- ^ a b c Ramsay, Gavin; Schreiber, Matthias R; Gänsicke, Boris T; Wheatley, Peter J (2017). "Distances of cataclysmic variables and related objects derived from Gaia Data Release 1". Astronomy & Astrophysics. 604: A107. arXiv:1704.00496. Bibcode:2017A&A...604A.107R. doi:10.1051/0004-6361/201730679. S2CID 56464882.
- ^ a b c d e f g Gilliland, R. L. (December 1982). "A time-resolved spectroscopic study and modeling of the dwarf nova BV Centauri". Astrophysical Journal. 263: 302–311. Bibcode:1982ApJ...263..302G. doi:10.1086/160504.
- ^ a b c d Sion, Edward M; Godon, Patrick; Cheng, Fuhua; Szkody, Paula (August 2007). "FUSE Observations of the Dwarf Novae UU Aql, BV Cen, and CH UMa in Quiescence". The Astronomical Journal. 134 (2): 886–895. arXiv:0704.1133. Bibcode:2007AJ....134..886S. doi:10.1086/518829. S2CID 14393007.
- ^ "V* BV Cen -- Dwarf Nova". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-11-07.
- ^ a b Plummer, A; Horn, P (June 2009). "The Changing Nature of the Dwarf Nova BV Centauri". The Journal of the American Association of Variable Star Observers. 37 (1): 23. Bibcode:2009JAVSO..37...23P.
- ^ Xu, Xiao-jie; Yu, Zhuo-li; Li, Xiang-Dong (2019). "The Fe Line Flux Ratio as a Diagnostic of the Maximum Temperature and the White Dwarf Mass of Cataclysmic Variables". The Astrophysical Journal. 878 (1): 53. arXiv:1905.03399. Bibcode:2019ApJ...878...53X. doi:10.3847/1538-4357/ab1fe1. S2CID 148571913.
- ^ Menzies, J. W; Odonoghue, D; Warner, B (May 1986). "BV Centauri - Dwarf or classical nova?". Astrophysics and Space Science. 122 (1): 73–80. Bibcode:1986Ap&SS.122...73M. doi:10.1007/BF00654382. S2CID 123400202.
