 Visual bandlight curves for QS Virginis, adapted from O’Donoghueet al. (2003).[1] The lowest plot shows two pre-eclipse dips. | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Virgo |
| Right ascension | 13h 49m 52.0032s[2] |
| Declination | −13° 13′ 37.002″[2] |
| Apparent magnitude (V) | +14.8 |
| Characteristics | |
| Spectral type | DAm / M3.5V |
| Astrometry | |
| Proper motion (μ) | RA: 41.618±0.108[2]mas/yr Dec.: 17.984±0.097[2]mas/yr |
| Parallax (π) | 19.9632±0.0584 mas[2] |
| Distance | 163.4 ± 0.5 ly (50.1 ± 0.1 pc) |
| Absolute magnitude (MV) | 11.74 + 11.82[1] |
| Orbit | |
| Period (P) | 217.092min[1] |
| Semi-major axis (a) | 0.0056AU |
| Eccentricity (e) | 0.0 |
| Inclination (i) | 60[1]° |
| Details[1] | |
| White dwarf | |
| Mass | 0.78 M☉ |
| Radius | 0.011 R☉ |
| Luminosity | 0.0044[3] 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[3] L☉ |
| Temperature | 3,100 K |
| Rotational velocity (v sin i) | 140 km/s |
| Other designations | |
| GSC 05559-00143,1RXS J134951.0-131338, WD 1347-129, EC 13471-1258, SBC9 1944[4] | |
| Database references | |
| SIMBAD | data |
QS Virginis (abbreviatedQS Vir) is aneclipsing binary system approximately 163light-years away from theSun,[1][2] forming acataclysmic variable. The system comprises an eclipsingwhite dwarf andred dwarf that orbit each other every 3.62hours.[1]
The eclipsing binary nature of QS Virginis was discovered in 1997 during theEdinburgh-Cape Blue Object Survey for blue stellar objects in the southern hemisphere.[5]
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.[6] The planet was announced to have aminimum mass 6.4 times the mass ofJupiter, in an elliptical orbit 4.2Astronomical 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 0.05solar masses (about 50 times the mass of Jupiter) in a highly eccentric 14-year orbit, making it abrown dwarf instead.[7]
