Astronomy:RX Andromedae

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Short description: Cataclysmic variable star system in the constellation Andromeda
RX Andromedae
RXAndLightCurve.png
The visual band light curve of RX Andromedae, from AAVSO data[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Andromeda
Right ascension  01h 04m 35.53730s[2]
Declination +41° 17′ 57.78369″[2]
Apparent magnitude (V) 10.2 to 15.1[3]
Characteristics
Spectral type pec(UG)[3]
B−V color index -0.4556[4]
Variable type UGZ[3]
Astrometry
Radial velocity (Rv)-12[5] km/s
Proper motion (μ) RA: 1.217 ± 2.221[6] mas/yr
Dec.: -22.225 ± 0.699 [6] mas/yr
Parallax (π)5.0276 ± 0.0507[2] mas
Distance649 ± 7 ly
(199 ± 2 pc)
Orbit
Period (P)5.075[7] hours
Details
White dwarf
Mass0.8[8] M☉
Surface gravity (log g)8.2[8] cgs
Temperature40,000 - 45,000[8] K
Rotational velocity (v sin i)200[8] km/s
Donor star
Surface gravity (log g)4.5[9] cgs
Temperature3,500[9] K
Metallicity+0.07[9]
Other designations
2MASS J01043553+4117577, TYC 2807-1623-1
Database references
SIMBADdata

RX Andromedae is a variable star in the constellation of Andromeda. Although it is classified as a dwarf nova of the Z Camelopardalis (UGZ) type, it has shown low-luminosity periods typical of VY Sculptoris stars.[10] However, for most of the time it varies from an apparent visual magnitude of 15.1 at minimum brightness to a magnitude of 10.2 at maximum brightness, with a period of approximately 13 days.[3]

System

RX Andromedae is a cataclysmic variable system, where a white dwarf with a mass of 0.8 M☉ and an M2 main sequence star[9] are rotating around their center of mass. The main sequence star is overfilling its Roche lobe, so the white dwarf is stripping away matter from the companion star and accreting it through an accretion disk.[10]

Variability

Like the Z Camelopardalis variables, RX Andromedae shows some periods of roughly constant luminosity and others where its brightness oscillates between a magnitude of 10.2 at its maximum and one of 15.1 at its minimum. However, between 1996 and 1997 it was stuck at its minimum brightness like cataclysmic variables of VY Sculptoris type, before going back to the usual behaviour. This places RX Andromedae in a transitional state between those two kind of objects.[10] The white dwarf and its accretion disk seems to be entirely responsible for this variability, and it's driven by changes in the accretion rate of the white dwarf.[8]

Spectrum

RX Andromedae has been extensively studied in optical and ultraviolet. It's also one of the few dwarf nova systems that have been detected at radio wavelengths.[11]

References

  1. ↑ "Download Data". AAVSO. https://www.aavso.org/data-download. 
  2. ↑ 2.0 2.1 2.2 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. 
  3. ↑ 3.0 3.1 3.2 3.3 RX And, database entry, Combined General Catalog of Variable Stars (GCVS4.2, 2004 Ed.), N. N. Samus, O. V. Durlevich, et al., CDS ID II/250 Accessed on line 2009-06-30.
  4. ↑ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P. et al. (2000), "The Tycho-2 catalogue of the 2.5 million brightest stars", Astronomy & Astrophysics 355: L27–L30, Bibcode: 2000A&A...355L..27H. 
  5. ↑ Kraft, R. P. (March 1962). "Binary Stars among Cataclysmic Variables. I. U Geminorum Stars (dwarf Novae).". Astrophysical Journal 135: 408. doi:10.1086/147280. Bibcode: 1962ApJ...135..408K. 
  6. ↑ 6.0 6.1 Gaia Collaboration; Brown, A. G. A; Vallenari, A; Prusti, T; De Bruijne, J. H. J; Mignard, F; Drimmel, R; Babusiaux, C et al. (2016). "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties". Astronomy & Astrophysics 595: A2. doi:10.1051/0004-6361/201629512. Bibcode: 2016A&A...595A...2G. 
  7. ↑ Kaitchuck, R. H. (1989), "The Orbital Period of RX Andromedae", Publications of the Astronomical Society of the Pacific 101: 1129, doi:10.1086/132587, Bibcode: 1989PASP..101.1129K. 
  8. ↑ 8.0 8.1 8.2 8.3 8.4 Sepinsky, J. F.; Sion, E. M.; Szkody, P.; Gänsicke, B. T. (2002), "Hubble Space Telescope Spectroscopy of the Dwarf Nova RX Andromedae during Outburst Rise and Decline", The Astrophysical Journal 574 (2): 937–941, doi:10.1086/341009, Bibcode: 2002ApJ...574..937S. 
  9. ↑ 9.0 9.1 9.2 9.3 Harrison, T. E. (2018), "The Identification of Hydrogen-deficient Cataclysmic Variable Donor Stars", The Astrophysical Journal 861 (2): 102, doi:10.3847/1538-4357/aacbd9, Bibcode: 2018ApJ...861..102H. 
  10. ↑ 10.0 10.1 10.2 Schreiber, M. R.; Gänsicke, B. T.; Mattei, J. A. (2002), "RX And: An intermediate between Z Cam and VY Scl stars", Astronomy and Astrophysics 384: L6–L9, doi:10.1051/0004-6361:20020122, Bibcode: 2002A&A...384L...6S. 
  11. ↑ Coppejans, D. L.; Körding, E. G.; Miller-Jones, J. C. A.; Rupen, M. P.; Sivakoff, G. R.; Knigge, C.; Groot, P. J.; Woudt, P. A. et al. (2016). "Dwarf nova-type cataclysmic variable stars are significant radio emitters". Monthly Notices of the Royal Astronomical Society 463 (2): 2229–2241. doi:10.1093/mnras/stw2133. Bibcode: 2016MNRAS.463.2229C. 

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