VV Ursae Majoris
| Observation data Epoch J2000 Equinox J2000 | ||
|---|---|---|
| Constellation | Ursa Major | |
| Right ascension | 09h 38m 06.719s[2] | |
| Declination | +56° 01′ 07.29″[2] | |
| Apparent magnitude (V) | 10.19[3] | |
| Characteristics | ||
| Spectral type | A1.5–2V[4] + G5IV[5] | |
| Variable type | ||
| Absolute magnitude (MV) | 1.87[4] | |
Semi-amplitude (K1) (primary) 59.6[7] km/s | | |
| Details | ||
| Primary | ||
| Mass | 0.97[5] M☉ | |
| Radius | 1.35[5] R☉ | |
| Luminosity | 11.2[5] L☉ | |
| Surface gravity (log g) | 4.37[4] cgs | |
| Temperature | 9,090[5] K | |
| Secondary | ||
| Mass | 0.29[5] M☉ | |
| Radius | 0.96[5] R☉ | |
| Luminosity | 0.42[5] L☉ | |
| Surface gravity (log g) | 4.00[4] cgs | |
| Temperature | 4,740[5] K | |
GCRV 6211[8] | ||
| Database references | ||
| SIMBAD | data | |
VV Ursae Majoris is a
This star was found to be
semidetached binary with the secondary component being significantly less massive than the primary.[11] In 1996, V. Simon found a periodic variation in the system minima with a cycle length of 22 years. He proposed that this variation is being driven by a third component in the system.[9]
This is an
subgiant star that is filling its Roche lobe.[11] The system displays an intrinsic low amplitude variability, which is probably coming from the primary.[4] Multiple pulsation periods have been detected.[12] There is no evidence of an infrared excess.[4]
The
mass of the Sun and is orbiting at a distance of 10.75 AU from the inner pair with an eccentricity of 0.35 and a period of 23.22±0.17 years.[13]
References
- ^ MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, retrieved 17 September 2022.
- ^ .
- ^ S2CID 119257644.
- ^ S2CID 119711271.
- ^ .
- ^ S2CID 125853869.
- ^ doi:10.1086/111159. See row 19, table 1, p. 540.
- ^ "VV UMa". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2022-09-16.
- ^ Bibcode:1996A&A...311..915S.
- doi:10.1086/145326.
- ^ Bibcode:1977A&AS...27..285B.
- Bibcode:2015IBVS.6148....1G.
- .
Further reading
- Ulas, Burak; et al. (August 2007), "The Algol-type Binary VV UMa: New VRI Photometry and Search for Pulsations", JENAM-2007, "Our non-stable Universe", held 20–25 August 2007 in Yerevan, Armenia, p. 21, Bibcode:2007jena.confE..21U, 21-21.
- Kim, S. -L.; et al. (February 2005), "On a short-periodic pulsating component in the Algol-type eclipsing binary system VV UMa", Information Bulletin on Variable Stars, 5598: 1, Bibcode:2005IBVS.5598....1K.
- Lázaro, C.; et al. (August 2001), "uvbyβ photometry of the short-period binary VV Ursae Majoris", Monthly Notices of the Royal Astronomical Society, 325 (2): 617–630, .
- Simon, Vojtech (1997), Leung, Kam-Ching (ed.), "Period Changes of the Binary VV UMa: Light-Time Effect or Magnetic Activity", The Third Pacific Rim Conference on Recent Development on Binary Star Research. Proceedings of a conference sponsored by Chiang Mai University, Thai Astronomical Society and the University of Nebraska-Lincoln held in Chiang Mai, Thailand, 26 October -1 November 1995, ASP Conference Series, vol. 130, p. 277, Bibcode:1997ASPC..130..277S.
- Simon, V. (July 1996), "The cyclic period changes of the close binary VV Ursae Majoris", Astronomy and Astrophysics, 311: 915–918, Bibcode:1996A&A...311..915S.
- Wunder, E. (March 1995), "The First Period Change Discovered in the Bright Algol System UV Leonis", Information Bulletin on Variable Stars, 4179: 1, Bibcode:1995IBVS.4179....1W.
- Horák, T. (1966), "New elements of the eclipsing variables TW Draconis, RW Tauri and KR Cygni and the influence of the rectification of the light curve upon the elements VV Ursae Maioris", Bulletin of the Astronomical Institute of Czechoslovakia, 17: 272, Bibcode:1966BAICz..17..272H.
- Wilson, Robert E. (June 1965), "A possible extended atmosphere in the eclipsing system W UMa", Astronomical Journal, 70: 368, doi:10.1086/109749.
