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]
Distance2,200 ± 100 ly
(690 ± 40 pc)
Details
Mass0.490±0.014[5] M☉
Radius0.17±0.01[5] R☉
Luminosity25.86+3.28
−2.61[5] L☉
Surface gravity (log g)5.83±0.01[4] cgs
Temperature34,850±90[4] K
Rotation24.6±3.5 d[5]
Other designations
UY Sex, GSC 04914-00003, 2MASS J10500281-0000369[6]
Database references
SIMBADdata

PG 1047+003 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]

References

  1. 1 2 3 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.
  2. 1 2 3 4 5 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.
  3. ↑ 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.
  4. 1 2 3 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.
  5. 1 2 3 4 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.
  6. ↑ "UY Sex". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2022-01-26.{{cite web}}: CS1 maint: postscript (link)
  7. ↑ 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.
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