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QS Telescopii is a faint, well-studied[4] binary star system in the southern constellation Telescopium.[7] It is composed of a white dwarf and main sequence donor star, locked into a close, circular orbit facing one another. Known as polars, material from the donor star does not form an accretion disk around the white dwarf, but rather streams directly onto it.[6] This is due to the presence of the white dwarf's strong magnetic field. The pair undergo frequent shifts between a high and low accretion states, and it shifts between single and double accretion poles. The main pole is partially self-eclipsing.[4]

QS Telescopii

A visual band light curve for QS Telescopii, adapted from Rosen et al. (1996)[1]
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Telescopium
Right ascension 19h 38m 35.816s[2]
Declination −46° 12 57.11[2]
Characteristics
Spectral type M4.5±0.5[3]
Variable type AM Her[4]
Astrometry
Radial velocity (Rv)110 km/s
Proper motion (μ) RA: +35.150 mas/yr[2]
Dec.: −25.496 mas/yr[2]
Parallax (π)5.3378 ± 0.0834 mas[2]
Distance611 ± 10 ly
(187 ± 3 pc)
Orbit[5]
Period (P)2.33 h
Eccentricity (e)0.0
Details
White Dwarf
Mass0.71[6] M
Temperature17,500[6] K
Other designations
QS Tel, EUVE J1938-46.2, RE 1938-461, AAVSO 1931-46[7]
Database references
SIMBADdata

The pair orbit each other with a period of 2.33[5] hours in a circular orbit. The donor star is a small red dwarf with an estimated stellar classification of M4−5.[3] The white dwarf primary has 71% of the mass of the Sun and an effective temperature of 17,500 K.[6] It has a magnetic field strength of 50–80 MG. The system is a source for X-ray emission.[4]


See also



References


  1. Rosen, S. R.; Mittaz, J. P. D.; Buckley, D. A.; Layden, A. C.; Clayton, K. L.; McCain, C.; Wynn, G. A.; Sirk, M. M.; Osborne, J. P.; Watson, M. G. (June 1996). "Accretion mode changes in QS Tel (RE 1938 — 461): EUVE, ROSAT and optical observations". Monthly Notices of the Royal Astronomical Society. 280 (4): 1121–1142. doi:10.1093/mnras/280.4.1121. Retrieved 13 April 2022.
  2. 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. Knigge, Christian (December 2006). "The donor stars of cataclysmic variables". Monthly Notices of the Royal Astronomical Society. 373 (2): 484–502. arXiv:astro-ph/0609671. Bibcode:2006MNRAS.373..484K. doi:10.1111/j.1365-2966.2006.11096.x.
  4. Traulsen, I.; Reinsch, K.; Schwope, A. D.; Burwitz, V.; et al. (2011). "XMM-Newton observations of the X-ray soft polar QS Telescopii". Astronomy and Astrophysics. 529 (A116): 7. arXiv:1103.4575. Bibcode:2011A&A...529A.116T. doi:10.1051/0004-6361/201016352. S2CID 119187792.
  5. Augusteijn, T.; et al. (June 2010). "Cataclysmic variables from the Calán-Tololo Survey - II. Spectroscopic periods". Monthly Notices of the Royal Astronomical Society. 405 (1): 621–637. Bibcode:2010MNRAS.405..621A. doi:10.1111/j.1365-2966.2010.16487.x.
  6. Gerke, Jill R.; et al. (2006). "Polars Changing State: Multiwavelength Long‐Term Photometry and Spectroscopy of QS Telescopii, V834 Centauri, and BL Hydri". Publications of the Astronomical Society of the Pacific. 118 (843): 678–86. arXiv:astro-ph/0603097. Bibcode:2006PASP..118..678G. doi:10.1086/503753. S2CID 14857705.
  7. "QS Tel". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-11-25.

Further reading





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