UY Sextantis
(Redirected from PG 1047+003)
 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) | 13.47 |
| Characteristics | |
| Spectral type | sdO9VII:He6[3] |
| Variable type | V361 Hya[1] |
| Astrometry | |
| Radial velocity (Rv) | 13.6[4] 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[5] M☉ |
| Radius | 0.17±0.01[5] R☉ |
| Luminosity | 25.86+3.28 −2.61[5] L☉ |
| Surface gravity (log g) | 5.83±0.01[4] cgs |
| Temperature | 34,850±90[4] K |
| Rotation | 24.6±3.5 d[5] |
| 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] No additional stellar companion has been detected in tight orbit or imaged around the subdwarf star.[7]
The star's variability was discovered in 1998 by D. O'Donoghue et al..[8] It was given its variable star designation in 2000.[9]
References
[edit]- ^ a b c Billeres; et al. (1997). "Discovery of p-mode Instabilities in the Hot Subdwarf B Star PG 1047+003". Astrophysical Journal Letters. 487 (1): 81–84. Bibcode:1997ApJ...487L..81B. doi:10.1086/310882.
- ^ a b c d Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ Drilling, J. S.; et al. (2013). "An MK-like system of spectral classification for hot subdwarfs". Astronomy & Astrophysics. 551: A31. Bibcode:2013A&A...551A..31D. doi:10.1051/0004-6361/201219433.
- ^ a b c Lei, Zhenxin; et al. (November 2018). "New Hot Subdwarf Stars Identified in Gaia DR2 with LAMOST DR5 Spectra". The Astrophysical Journal. 868 (1): 9. arXiv:1810.09625. Bibcode:2018ApJ...868...70L. doi:10.3847/1538-4357/aae82b. S2CID 250892206. 70.
- ^ a b c d Reed, M. D.; et al. (March 2020). "K2 observations of the pulsating subdwarf B stars UY Sex and V1405 Ori". Monthly Notices of the Royal Astronomical Society. 492 (4): 5202–5217. Bibcode:2020MNRAS.492.5202R. doi:10.1093/mnras/staa144.
- ^ "UY Sex". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2022-01-26.
{{cite web}}: CS1 maint: postscript (link) - ^ O'Donoghue; Koen; Lynas-Gray; Kilkenny; Van Wyk (1998). "The EC14026 stars - VI. PG1047+003". Monthly Notices of the Royal Astronomical Society. 296 (2): 306–316. Bibcode:1998MNRAS.296..306O. doi:10.1046/j.1365-8711.1998.01311.x.
- ^ O'Donoghue, D.; Koen, C.; Lynas-Gray, A. E.; Kilkenny, D.; van Wyk, F. (May 1998). "The EC14026 stars - VI. PG1047+003". Monthly Notices of the Royal Astronomical Society. 296 (2): 306–316. Bibcode:1998MNRAS.296..306O. doi:10.1046/j.1365-8711.1998.01311.x.
- ^ Kazarovets, E. V.; Samus, N. N.; Durlevich, O. V. (March 2000). "The 75th Name-List of Variable Stars" (PDF). Information Bulletin on Variable Stars. 4870: 1. Bibcode:2000IBVS.4870....1K. Retrieved 11 October 2024.
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