Astronomy:TW Pictoris
 A light curve for TW Pictoris. The main plot,adapted from Scaringi et al. (2021),[1] shows the long-term visual band variation, and the inset plot, adapted from Patterson and Moulden (1993),[2] shows the periodic variability. | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Pictor |
| Right ascension | 05h 34m 50.586s[3] |
| Declination | −58° 01′ 40.77″[3] |
| Apparent magnitude (V) | 15.10[4] (14.1 - 15.6)[5] |
| Characteristics | |
| U−B color index | 0.99[4] |
| B−V color index | 0.27[4] |
| Variable type | Nova-like variable[6] |
| Astrometry | |
| Proper motion (μ) | RA: −11.632[3] mas/yr Dec.: 3.745[3] mas/yr |
| Parallax (π) | 2.2839 ± 0.0223[3] mas |
| Distance | 1,430 ± 10 ly (438 ± 4 pc) |
| Other designations | |
| Database references | |
| SIMBAD | data |
TW Pictoris is a 14th magnitude cataclysmic variable star system in the southern constellation of Pictor. It is located at a distance of approximately 1,430 light-years based on parallax measurements. Photometric observations in the visual band suggest a binary system with an orbital period of 6.06 hours.[8] One of the components is an accreting white dwarf.[1]
The X-ray source H0534-581 was identified from the data collected by the HEAO 1 satellite in 1979. In 1984, a candidate optical counterpart was identified by I. R. Tuohy and associates from photographs taken at the Schmidt telescope. A low-resolution spectrum revealed this is a cataclysmic variable, and it was assigned the variable star designation TW Pictoris. It was initially proposed to be an intermediate polar,[9][10] but the lack of an X-ray pulsation makes this less likely.[11] The current classification remains controversial.[1]
References
- ↑ 1.0 1.1 1.2 Scaringi, S. et al. (October 2021). "An accreting white dwarf displaying fast transitional mode switching". Nature Astronomy 6: 98–102. doi:10.1038/s41550-021-01494-x. Bibcode: 2022NatAs...6...98S.
- ↑ Patterson, Joseph; Moulden, Margaret (July 1993). "Rapid Oscillations in Cataclysmic Variables. X. TW Pictoris (= H0534-581)". Publications of the Astronomical Society of the Pacific 105: 779–784. doi:10.1086/133229. Bibcode: 1993PASP..105..779P.
- ↑ 3.0 3.1 3.2 3.3 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 4.0 4.1 4.2 O'Donoghue, D. et al. (May 2013). "The Edinburgh-Cape Blue Object Survey - III. Zone 2; galactic latitudes -30° > b > -40°". Monthly Notices of the Royal Astronomical Society 431 (1): 240–251. doi:10.1093/mnras/stt158. Bibcode: 2013MNRAS.431..240O.
- ↑ Watson, Christopher (4 January 2010). "TW Pictoris". AAVSO Website. American Association of Variable Star Observers. http://www.aavso.org/vsx/index.php?view=detail.top&oid=26363. Retrieved 28 July 2014.
- ↑ Samus, N. N. et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports. 5.1 61 (1): 80–88. doi:10.1134/S1063772917010085. Bibcode: 2017ARep...61...80S. http://www.sai.msu.su/gcvs/gcvs/. Retrieved 2021-11-27.
- ↑ "TW Pic". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=TW+Pic.
- ↑ Balman, S.; Talebpour-Sheshvan, N.; Nabizadeh, A. (June 2016). "XMM-Newton Observations of TW PIC in comparison with the Archival SWIFT and RXTE data". XMM-Newton: The Next Decade, Proceedings of the Conference held 9-11 May, 2016 at ESAC, Madrid. 73. Bibcode: 2016xnnd.confE..73B.
- ↑ Tuohy, I. R. et al. (December 1986). "Identification of two southern X-ray emitting cataclysmic variables". Astrophysical Journal 311: 275–298. doi:10.1086/164770. Bibcode: 1986ApJ...311..275T.
- ↑ Mouchet, M. et al. (October 1991). "The UV variability of the intermediate polars TW Pictoris (H 0534-581) and TX Columbae (1H 0542-407)". Astronomy and Astrophysics 250: 99. Bibcode: 1991A&A...250...99M.
- ↑ Norton, A. J. et al. (February 2000). "The nature of TW Pictoris". Monthly Notices of the Royal Astronomical Society 312 (2): 362–370. doi:10.1046/j.1365-8711.2000.03216.x. Bibcode: 2000MNRAS.312..362N.
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