Astronomy:DW Ursae Majoris

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Short description: Variable star in the constellation Ursa Major
DW Ursae Majoris
DWUMaLightCurve.png
A light curve for DW Ursae Majoris, plotted from TESS data[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Ursa Major
Right ascension  10h 33m 52.875s[2]
Declination +58° 46′ 54.72″[2]
Apparent magnitude (V) 13.6 to 18.0[3]
Characteristics
Spectral type M7±2.0[4]
Variable type Algol variable[5]
Astrometry
Proper motion (μ) RA: 0.974[2] mas/yr
Dec.: 1.396[2] mas/yr
Parallax (π)1.6958 ± 0.0196[2] mas
Distance1,920 ± 20 ly
(590 ± 7 pc)
Orbit
Period (P)3.2785566 h[3]
Semi-major axis (a)1.14±0.06 R☉[4]
Inclination (i)82±4[4]°
Details
White dwarf
Mass0.77±0.07[4] M☉
Radius0.012±0.001[4] R☉
Surface gravity (log g)8[4] (assumed) cgs
Temperature50,000±1,000[4] K
Red dwarf
Mass0.25±0.05[6] M☉
Radius0.34±0.04[4] R☉
Other designations
PG 1030+590, DW UMa, GSC 03822-00464, 2MASS J10335283+5846547[7]
Database references
SIMBADdata

DW Ursae Majoris is an eclipsing binary star system in the northern circumpolar constellation of Ursa Major, abbreviated DW UMa. It is a cataclysmic variable of the SX Sextanis type, consisting of a compact white dwarf that is accreting matter from an orbiting companion star.[8] The brightness of this source ranges from an apparent visual magnitude of 13.6 down to magnitude 18,[5] which is too faint to be viewed with the naked eye. The distance to this system is approximately 1,920 light years based on parallax measurements.[2]

In 1982, R. F. Green and associates identified this star as a cataclysmic variable candidate with the Palomar–Green survey designation PG 1030+590.[9] A. W. Shafter and F. V. Hessman in 1984 found this to be a close eclipsing binary system with a period of 3.27 hours.[10] This is a nova-like binary where mass is being transferred from a late-type star to a white dwarf companion. This material is first accumulated in an accretion disk orbiting the white dwarf. Typically, the light curve for an eclipsing binary of this type should display a hump-like feature from where the stream of material interacts with the disk. However, during early observations, no such feature was observed before the eclipse.[11]

The behavior of the emission lines in the spectrum of this star were found to resemble those of other SW Sextantis variables.[12] In 2000, the system was observed with the Hubble Space Telescope and was found to be in a low state about three magnitudes fainter, unlike previous observations where it had been in a high state. Comparison of the ultraviolet spectrum in the two states suggested that the accretion disk is self-eclipsing and it can obscure the view of the white dwarf.[8] The light output of the system undergoes a 13.6 year cycle of variation, probably because of precession of the accretion disk. Both positive and negative superhumps are observed that vary over time in a complex fashion. Mass is being transferred from the donor star at a rate of about 10−8 M☉·yr−1.[6]

References

  1. ↑ MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html, retrieved 16 October 2022. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G.  Gaia EDR3 record for this source at VizieR.
  3. ↑ 3.0 3.1 DW UMa, AAVSO, https://www.aavso.org/vsx/index.php?view=detail.top&oid=37249, retrieved 2022-10-14. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 4.6 4.7 Araujo-Betancor, S. et al. (January 2003), "The System Parameters of DW Ursae Majoris", The Astrophysical Journal 583 (1): 437–445, doi:10.1086/345098, Bibcode: 2003ApJ...583..437A. 
  5. ↑ 5.0 5.1 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. 
  6. ↑ 6.0 6.1 Boyd, D. R. S. et al. (April 2017), "A 16-yr photometric campaign on the eclipsing novalike variable DW Ursae Majoris", Monthly Notices of the Royal Astronomical Society 466 (3): 3417–3433, doi:10.1093/mnras/stw3327, Bibcode: 2017MNRAS.466.3417B. 
  7. ↑ "DW UMa". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=DW+UMa. 
  8. ↑ 8.0 8.1 Knigge, Christian et al. (August 2000), "A Self-occulting Accretion Disk in the SW Sextantis Star DW Ursae Majoris", The Astrophysical Journal 539 (1): L49–L53, doi:10.1086/312825, Bibcode: 2000ApJ...539L..49K. 
  9. ↑ Green, R. F. et al. (June 1982), "Cataclysmic variable candidates from the Palomar Green Survey", Publications of the Astronomical Society of the Pacific 94: 560-564, doi:10.1086/131022, Bibcode: 1982PASP...94..560G. 
  10. ↑ Shafter, A. W.; Hessman, F. V. (1984), "Time resolved spectroscopy and photometry of a new eclipsing cataclysmic variable, PG 1030+590", Bulletin of the American Astronomical Society 16: 505, Bibcode: 1984BAAS...16R.505S. 
  11. ↑ Szkody, Paula (October 1987), "Time-Resolved IUE Studies of Cataclysmic Variables. I. Eclipsing Systems of IP Peg, PG 1030 + 590, and V1315 AQL", Astronomical Journal 94: 1055, doi:10.1086/114540, Bibcode: 1987AJ.....94.1055S. 
  12. ↑ Thorstensen, John R. et al. (August 1991), "A Spectroscopic Study of the Eclipsing Cataclysmic Binary Star PG0818+513: A Puzzling Novalike Variable", Astronomical Journal 102: 683, doi:10.1086/115902, Bibcode: 1991AJ....102..683T. 

Further reading

  • Smak, J. (September 2017), "DW UMa and the Irradiation Modulated Mass Transfer Model for Superhumps", Acta Astronomica 67 (3): 273–280, doi:10.32023/0001-5237/67.3.5, Bibcode: 2017AcA....67..273S. 
  • Sanad, M. R. (February 2014), "Ultraviolet spectral behavior of IP Peg and DW UMa in high, intermediate and low states from the HST and IUE satellites", New Astronomy 27: 63–72, doi:10.1016/j.newast.2013.09.003, Bibcode: 2014NewA...27...63S. 
  • Hoard, D. W. et al. (November 2010), "Simultaneous X-ray and Ultraviolet Observations of the SW Sextantis Star DW Ursae Majoris", The Astronomical Journal 140 (5): 1313–1320, doi:10.1088/0004-6256/140/5/1313, Bibcode: 2010AJ....140.1313H. 
  • Boyd, D. (August 2008), "Observing DW UMa - a very active variable star", Journal of the British Astronomical Association 118 (4): 222, Bibcode: 2008JBAA..118..222B. 
  • Ostrova, N. I. et al. (April 2005), "Wavelength Dependence of the Orbital Variability of the Eclipsing Nova-Like Object DW UMa", Astrophysics and Space Science 296 (1–4): 473–476, doi:10.1007/s10509-005-4894-0, Bibcode: 2005Ap&SS.296..473O. 
  • Knigge, Christian et al. (November 2004), "Time-resolved Ultraviolet Spectroscopy of the SW Sex Star DW UMa: Confirmation of a Hidden White Dwarf and the Ultraviolet Counterpart to Phase 0.5 Absorption Events", The Astrophysical Journal 615 (2): L129–L132, doi:10.1086/426118, Bibcode: 2004ApJ...615L.129K. 
  • Stanishev, V. et al. (March 2004), "Accretion disc evolution in DW Ursae Majoris: A photometric study", Astronomy and Astrophysics 416 (3): 1057–1067, doi:10.1051/0004-6361:20034145, Bibcode: 2004A&A...416.1057S. 
  • Hoard, D. W. et al. (November 2003), "Observations of the SW Sextantis Star DW Ursae Majoris with the Far Ultraviolet Spectroscopic Explorer", The Astronomical Journal 126 (5): 2473–2486, doi:10.1086/378605, Bibcode: 2003AJ....126.2473H. 
  • Bíró, I. B. (January 2002), Gänsicke, B. T.; Beuermann, K.; Reinsch, K., eds., "Photometric followup of DW UMa", The Physics of Cataclysmic Variables and Related Objects, ASP Conference Proceedings (San Francisco: Astronomical Society of the Pacific) 261: 469, ISBN 1-58381-101-X, Bibcode: 2002ASPC..261..469B. 
  • Bíró, I. B. (December 2000), "Eclipse mapping of the cataclysmic variable DW Ursae Majoris", Astronomy and Astrophysics 364: 573–586, Bibcode: 2000A&A...364..573B. 
  • Bíró, I. B. (1998), Dusek, J., ed., "CCD Photometry of the Eclipsing Nova-like Variable DW Ursae Majoris", Proceedings of the 20th Stellar Conference of the Czech and Slovak Astronomical Institutes. 5th - 7th November 1997. Brno, Czech Republic (Brno): p. 30, ISBN 80-85882-08-6, Bibcode: 1998vsr..conf...30B. 
  • Dhillon, V. S. et al. (February 1994), "Observations of the eclipsing nova-like variable DW Ursae Majoris in a low state", Monthly Notices of the Royal Astronomical Society 266 (4): 859–871, doi:10.1093/mnras/266.4.859, Bibcode: 1994MNRAS.266..859D. 
  • Honeycutt, R. K. et al. (September 1993), "The Long-Term Light Curve of the Cataclysmic Variable DW Ursae Majoris", Publications of the Astronomical Society of the Pacific 105: 922, doi:10.1086/133256, Bibcode: 1993PASP..105..922H. 
  • Kazennova, E. A.; Shugarov, S. Yu. (1992), Vogt, Nikolaus, ed., "The Photometry and Analysis of the Light Curves of the Cataclysmic Variables AY PSC and DW UMa", Vina del Mar Workshop on Cataclysmic Variable Stars, ASP Conference Series (San Francisco: Astronomical Society of the Pacific) 29: p. 390, Bibcode: 1992ASPC...29..390K. 
  • Green, R. F. et al. (August 1991), "Cataclysmic variable candidates from the Palomar Green Survey", Astronomical Journal 102: 683, doi:10.1086/115902, Bibcode: 1991AJ....102..683T. 
  • Szkody, Paula; Piche, Francois (September 1990), "The Phase 0.5 Absorption in V1315 Aquilae, SW Sextantis, and DW Ursae Majoris", Astrophysical Journal 361: 235, doi:10.1086/169188, Bibcode: 1990ApJ...361..235S. 
  • Hessman, F. V. (February 1990), Green, D. W. E., ed., "DW Ursae Majoris", IAU Circular 4971: 1, Bibcode: 1990IAUC.4971....1H. 
  • Andronov, I. L. et al. (October 1989), "Detection of the 224-min Orbital Period of the Cataclysmic Variable PG 0818+513", Information Bulletin on Variable Stars 3388: 1, Bibcode: 1989IBVS.3388....1A. 
  • Shafter, A. W. et al. (April 1988), "Photometric and Spectroscopic Observations of the Eclipsing Nova-like Variable PG 1030+590 (DW Ursae Majoris)", Astrophysical Journal 327: 248, doi:10.1086/166186, Bibcode: 1988ApJ...327..248S. 




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