QS Virginis
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Virgo |
| Right ascension | 13h 49m 51.95s |
| Declination | −13° 13′ 37.5″ |
| Apparent magnitude (V) | +14.8 |
| Characteristics | |
| Spectral type | DAm / M3.5V |
| Astrometry | |
| Distance | 156.48 ly (48±5[1] pc) |
| Absolute magnitude (MV) | 11.74 + 11.82[1] |
| Orbit | |
| Period (P) | 217.092 min[1] |
| Semi-major axis (a) | 0.0056 AU |
| Eccentricity (e) | 0.0 |
| Inclination (i) | 60[1]° |
| Details[1] | |
| White dwarf | |
| Mass | 0.78 M☉ |
| Radius | 0.011 R☉ |
| Luminosity | 0.0044[2] L☉ |
| Surface gravity (log g) | 8.34 cgs |
| Temperature | 14,200 K |
| Rotational velocity (v sin i) | 400 km/s |
| Red dwarf | |
| Mass | 0.43 M☉ |
| Radius | 0.42 R☉ |
| Luminosity | 0.015[2] L☉ |
| Temperature | 3,100 K |
| Rotational velocity (v sin i) | 140 km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| Extrasolar Planets Encyclopaedia | data |
QS Virginis (abbreviated QS Vir) is an eclipsing binary system approximately 157 light-years away from the Sun,[1] forming a cataclysmic variable. The system comprises an eclipsing white dwarf and red dwarf that orbit each other every 3.37 hours.[1]
Possible third body
In 2009 the discovery of an extrasolar planet in orbit around the binary star was announced, detected by variations in the timings of the eclipses of the two stars.[3] The planet was announced to have a minimum mass 6.4 times the mass of Jupiter, in an elliptical orbit 4.2 Astronomical Units away from binary.
Subsequent observations revealed that the timings were not following the pattern predicted by the planetary model. While the observed variations in eclipse times may be caused by a third body, the best fit model orbit is for an object with minimum mass 0.05 solar masses (about 50 times the mass of Jupiter) in a highly eccentric 14-year orbit.[4]
See also
References
- 1 2 3 4 5 6 7 O'Donoghue; Koen, C.; Kilkenny, D.; Stobie, R. S.; et al. (2003). "The DA+dMe eclipsing binary EC13471-1258: its cup runneth over ... just". Monthly Notices of the Royal Astronomical Society. 345 (2): 506–528. arXiv:astro-ph/0307144. Bibcode:2003MNRAS.345..506O. doi:10.1046/j.1365-8711.2003.06973.x.
- 1 2 Calculated from the effective temperature and radius
- ↑ Qian, S.-B.; Liao, W.-P.; Zhu, L.-Y.; Dai, Z.-B.; et al. (2009). "A giant planet in orbit around a magnetic-braking hibernating cataclysmic variable". Monthly Notices of the Royal Astronomical Society. 401 (1): L34–L38. Bibcode:2010MNRAS.401L..34Q. doi:10.1111/j.1745-3933.2009.00780.x.
- ↑ Parsons, S. G.; Marsh, T. R.; Copperwheat, C. M.; Dhillon, V. S.; et al. (2010). "Orbital Period Variations in Eclipsing Post Common Envelope Binaries". Monthly Notices of the Royal Astronomical Society. 407 (4): 2362–2382. arXiv:1005.3958. Bibcode:2010MNRAS.407.2362P. doi:10.1111/j.1365-2966.2010.17063.x.
