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BZ Ursae Majoris

From Wikipedia, the free encyclopedia
Dwarf Nova in the constellation Ursa Major
BZ Ursae Majoris

Avisual bandlight curve for BZ Ursae Majoris. The main plot (fromAAVSO data[1]) shows several outbursts, and the inset plot (adapted from Katoet al.[2]) shows a single superoutburst in detail.
Observation data
Epoch J2000.0      Equinox J2000.0
ConstellationUrsa Major
Right ascension08h 53m 44.174s[3]
Declination+57° 48′ 40.59″[3]
Apparent magnitude (V)15.7 to 16.5[4]
10.2 to 15.9[5]
Characteristics
Spectral typeM5.5:Ve[6]
Variable typeSU UMa[7]
Astrometry
Proper motion (μ)RA: 26.318mas/yr[3]
Dec.: −15.915mas/yr[3]
Parallax (π)6.4561±0.0441 mas[3]
Distance505 ± 3 ly
(155 ± 1 pc)
Orbit[6]
Period (P)97.8±0.1 h
Inclination (i)~60[8]°
Periastronepoch (T)2,448,319.897±0.003 HJD
Details
White dwarf
Mass0.65[9][10] M☉
Radius6,880[11] km
Surface gravity (log g)7.5[5][12] cgs
Temperature15,000[5][12] K
Rotational velocity (v sin i)200[5] km/s
Donor star
Mass0.13[6] M☉
Other designations
BZ UMa,2MASS J08534416+5748406, PG 0849+580[13]
Database references
SIMBADdata

BZ Ursae Majoris is adwarf novastar system in the northerncircumpolar constellation ofUrsa Major. It consists of awhite dwarf primary in a close orbit with ared dwarf. The latter star is donating mass, which is accumulating in anaccretion disk orbiting the white dwarf.[14] The system is located at a distance of approximately 505 light years from theSun based onparallax measurements.[3]

This system was discovered to vary in brightness byB. E. Markaryan in 1968,[15] and it was given thevariable star designation BZ UMa.[16] After four years of observation by theAAVSO, it was proposed to be acataclysmic variable byM. Mayall.[14] In 1982,R. F. Green and associates identified it as a cataclysmic variable candidate of theU Gem-type, based on itsspectrum.[17] The same year,W. Wenzel showed that this star had very long intervals between outbursts, placing it intermediate between the U Gem andWZ Sge classes.[18]P. Szkody andL. Feinswog examined theinfraredlight curve of the system, estimating anorbital inclination of 60° with no evidence of heating from the white dwarf.[8]

R. Claudi and associates in 1990 found a periodic modulation of hydrogenemission lines, indicating anorbital period of1.62 h. They suggested it be classified as aSU UMa star.[19] Spectroscopic examination of the system using theHubble Space Telescope during 2001 showed an anomalous abundance ratio of nitrogen to carbon that indicatesCNO-processing.[20] This may be the result of an earlierevolutionary stage of the donor star that was stripped of its outer layers. Asuperoutburst was observed in 2007 that displayedsuperhumps. A lack ofcircular polarization indicates the white dwarf is not stronglymagnetic, and thus this system is most likely not anintermediate polar.[14]

References

[edit]
  1. ^"Download Data".aavso.org. AAVSO. Retrieved1 October 2021.
  2. ^Kato, Taichi; et al. (December 2009)."Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae".Publications of the Astronomical Society of Japan.61:S395 –S616.arXiv:0905.1757.Bibcode:2009PASJ...61S.395K.doi:10.1093/pasj/61.sp2.S395. Retrieved19 June 2022.
  3. ^abcdeBrown, A. G. A.; et al. (Gaia collaboration) (2021)."Gaia Early Data Release 3: Summary of the contents and survey properties".Astronomy & Astrophysics.649: A1.arXiv:2012.01533.Bibcode:2021A&A...649A...1G.doi:10.1051/0004-6361/202039657.S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source atVizieR.
  4. ^Heinze, A. N.; et al. (November 2018), "A First Catalog of Variable Stars Measured by the Asteroid Terrestrial-impact Last Alert System (ATLAS)",The Astronomical Journal,156 (5): 49,arXiv:1804.02132,Bibcode:2018AJ....156..241H,doi:10.3847/1538-3881/aae47f,S2CID 59939788, 241.
  5. ^abcdGodon, Patrick; et al. (September 2011), "A Far-Ultraviolet Spectroscopic Analysis of BZ Ursae Majoris",Publications of the Astronomical Society of the Pacific,123 (907): 1071,arXiv:1107.4790,Bibcode:2011PASP..123.1071G,doi:10.1086/661763,S2CID 119265399.
  6. ^abcRingwald, F. A.; et al. (November 1994), "Orbital studies of the cataclysmic variables CZ Orionis, V1193 Orionis and BZ Ursae Majoris",Monthly Notices of the Royal Astronomical Society,271 (2):323–342,Bibcode:1994MNRAS.271..323R,doi:10.1093/mnras/271.2.323.
  7. ^Vogt, N.; et al. (April 2021), "Determination of the superoutburst cycle lengths of 206 SU UMa-type dwarf novae",Monthly Notices of the Royal Astronomical Society,502 (4):5668–5678,arXiv:2101.02756,Bibcode:2021MNRAS.502.5668V,doi:10.1093/mnras/staa3711.
  8. ^abSzkody, Paula; Feinswog, Laurie (November 1988), "Infrared Light Curves of Three Novae and Three Dwarf Novae at Quiescence",Astrophysical Journal,334: 422,Bibcode:1988ApJ...334..422S,doi:10.1086/166846.
  9. ^Maccarone, Thomas J.; Arur, Kavitha (December 2019), "On the Mass of the White Dwarf in BZ UMa",Research Notes of the American Astronomical Society,3 (12): 185,Bibcode:2019RNAAS...3..185M,doi:10.3847/2515-5172/ab60ab,S2CID 216539831, 185.
  10. ^Yu, Zhuo-li; et al. (February 2018), "An Empirical Correlation of T max-M WD of Dwarf Novae and the Average White Dwarf Mass in Cataclysmic Variables in the Galactic Bulge",The Astrophysical Journal,853 (2): 8,arXiv:1804.00786,Bibcode:2018ApJ...853..182Y,doi:10.3847/1538-4357/aaa47d,S2CID 119364315, 182.
  11. ^İkis Gün, G.; et al. (December 2013), "Preliminary results of the spectral analysis of Suzaku data of SW Ursae Majoris and BZ Ursae Majoris",New Astronomy,25:1–6,Bibcode:2013NewA...25....1I,doi:10.1016/j.newast.2013.03.011.
  12. ^abSion, Edward M. (June 2012), "White Dwarfs in Cataclysmic Variable Stars: Surface Temperatures and Evolution",Journal of Astronomy and Space Sciences,29 (2):169–173,Bibcode:2012JASS...29..169S,doi:10.5140/JASS.2012.29.2.169.
  13. ^"BZ UMa",SIMBAD,Centre de données astronomiques de Strasbourg, retrieved2022-03-09.
  14. ^abcPrice, A.; et al. (November 2009), "Polarimetry and the Long-Awaited Superoutburst of BZ UMa",Publications of the Astronomical Society of the Pacific,121 (885): 1205,arXiv:0909.4024,Bibcode:2009PASP..121.1205P,doi:10.1086/648479,S2CID 118612829.
  15. ^Neustroev, V. V.; et al. (July 2004), Tovmassian, G.; E., Sion (eds.), "New spectroscopic observations of dwarf nova BZ Ursae Majoris with extremely unusual emission lines profiles",Compact Binaries in the Galaxy and Beyond, Proceedings of the conference held 17-22 November, 2003 in La Paz, Baja California Sur, IAU Colloquium 194, Revista Mexicana de Astronomía y Astrofísica (Serie de Conferencias), vol. 20, p. 269,Bibcode:2004RMxAC..20..269N.
  16. ^Kukarkin, B. V.; et al. (October 1970), "57th Name-List of Variable Stars",Information Bulletin on Variable Stars,480 (1): 1,Bibcode:1970IBVS..480....1K.
  17. ^Green, R. F.; Ferguson, D. H.; Liebert, J.; Schmidt, M. (June 1982), "Cataclysmic variable candidates from the Palomar Green Survey",Publications of the Astronomical Society of the Pacific,94:560–564,Bibcode:1982PASP...94..560G,doi:10.1086/131022,S2CID 120644760.
  18. ^Wenzel, W. (December 1982), "BZ Ursae Majoris - Missing Link Between the Dwarf Novae of U Geminorum and WZ Sagittae Type",Information Bulletin on Variable Stars,2256 (1): 1,Bibcode:1982IBVS.2256....1W.
  19. ^Claudi, R.; et al. (March 1990), Green, D. W. E. (ed.), "BZ Ursae Majoris",IAU Circular,4975 (2): 2,Bibcode:1990IAUC.4975....2C.
  20. ^Gänsicke, Boris T.; et al. (September 2003), "Anomalous Ultraviolet Line Flux Ratios in the Cataclysmic Variables 1RXS J232953.9+062814, CE 315, BZ Ursae Majoris, and EY Cygni, Observed with the Hubble Space Telescope Space Telescope Imaging Spectrograph",The Astrophysical Journal,594 (1):443–448,arXiv:astro-ph/0305264,Bibcode:2003ApJ...594..443G,doi:10.1086/376902,S2CID 120224177.

Further reading

[edit]
  • Sion, E. M.; Godon, P. (2012), "White dwarfs in cataclysmic variable stars: accretion physics and evolution",Memorie della Societa Astronomica Italiana,83: 539,Bibcode:2012MmSAI..83..539S.
  • Jiang, L. L.; et al. (January 2010), "The Photometry of Cataclysmic Variable V1159 Ori and BZ UMa",Acta Astronomica Sinica,51 (1):42–53,Bibcode:2010AcASn..51...42J.
  • Price, A.; et al. (May 2004), "Flickering and Periodic Activity in the 2004 Outburst of BZ UMa",Information Bulletin on Variable Stars,5526 (1): 1,Bibcode:2004IBVS.5526....1P.
  • Kato, T. (September 1999), "CCD Photometry of the 1999 March Outburst of BZ UMa: Detection of Quasi-Periodic Oscillations",Information Bulletin on Variable Stars,4768 (1): 1,Bibcode:1999IBVS.4768....1K.
  • Jurcevic, J. S.; et al. (May 1994), "Spectroscopy and Photometry of the Dwarf Nova BZ UMa and the CV Line-Width/K, Mass-Ratio Relation",Publications of the Astronomical Society of the Pacific,106: 481,Bibcode:1994PASP..106..481J,doi:10.1086/133403,S2CID 120863048.
  • Ringwald, F. A.; Thorstensen, J. R. (September 1990), "Quasi-Periodic Variation in the Radial Velocity Curve of the Dwarf Nova BZ UMa",Bulletin of the American Astronomical Society,22: 1291,Bibcode:1990BAAS...22.1291R.
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