 A white light light curve for UY Sextantis, adapted from Billeres et al. (1997). [1] All five panels form a single 10,000 second light curve, with the top panel continued on the second panel, etc. | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Sextans |
| Right ascension | 10h 50m 02.826s [2] |
| Declination | −00° 00′ 36.88″ [2] |
| Apparent magnitude (V) | 13.49 [3] |
| Characteristics | |
| Spectral type | sdO9VII:He6 [4] |
| Variable type | V361 Hya [1] |
| Astrometry | |
| Radial velocity (Rv) | 13.6 [5] km/s |
| Proper motion (μ) | RA: −20.528 mas/yr [2] Dec.: −38.421 mas/yr [2] |
| Parallax (π) | 1.4559 ± 0.0789 mas [2] |
| Distance | 2,200 ± 100 ly (690 ± 40 pc) |
| Details | |
| Mass | 0.490±0.014 [6] M☉ |
| Radius | 0.17±0.01 [6] R☉ |
| Luminosity | 25.86+3.28 −2.61 [6] L☉ |
| Surface gravity (log g) | 5.83±0.01 [5] cgs |
| Temperature | 34,850±90 [5] K |
| Rotation | 24.6±3.5 d [6] |
| Other designations | |
| Database references | |
| SIMBAD | data |
UY Sextantis is a post-AGB blue-white subdwarf star, located in the constellation of Sextans. The star is classed as member of the V361 Hydrae type (or also called sdBVr type) class of pulsators in the field of asteroseismology, [1] although it is now generally classified as class O. [4] No additional stellar companion has been detected in tight orbit or imaged around the subdwarf star. [8]
The star's variability was discovered in 1998 by D. O'Donoghue et al.. [9] It was given its variable star designation in 2000. [10] It has an apparent magnitude of 13.5 and the brightness changes amount to less than 0.1 magnitudes, [3] with a typical period of 142 seconds. [1]
