Astronomy:QQ Vulpeculae

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Short description: Variable star in the constellation Vulpecula
QQ Vulpeculae
QQVulLightCurve.png
A blue band light curve for QQ Vulpeculae, adapted from Nousek et al. (1984)[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Vulpecula
Right ascension  20h 05m 41.909s[2]
Declination 22° 39′ 58.84″[2]
Apparent magnitude (V) 14.656[3]
Characteristics
Spectral type M4V[4]
Apparent magnitude (B) 14.4 to 17.0[5]
Variable type Polar[5]
Astrometry
Proper motion (μ) RA: −3.249[2] mas/yr
Dec.: −14.882[2] mas/yr
Parallax (π)3.3235 ± 0.0286[2] mas
Distance981 ± 8 ly
(301 ± 3 pc)
Orbit[6]
Period (P)0.1545217±0.0000022 d
Semi-major axis (a)1.14±0.12 R☉[4]
Eccentricity (e)0.00
Inclination (i)≥ 72[7]°
Periastron epoch (T)2,445,234.8364±0.0018 JD
Semi-amplitude (K1)
(primary)		369.00 km/s
Semi-amplitude (K2)
(secondary)		219±6[4] km/s
Details
White dwarf
Mass0.58–0.66[7] M☉
Radius0.01[8] R☉
Donor star
Mass0.34–0.44[7] M☉
Radius0.35±0.10[4] R☉
Rotational velocity (v sin i)110±15[4] km/s
Other designations
E 2003+225, QQ Vul, IRAS J20054191+2239587[9]
Database references
SIMBADdata

QQ Vulpeculae is a cataclysmic variable binary star system in the northern constellation of Vulpecula, abbreviated QQ Vul. It has a brightness that fluctuates around an apparent visual magnitude of 14.7,[3] which is too faint to be viewed with the naked eye. The distance to this system is approximately 981 light years based on parallax measurements.[2]

This system was detected as a soft X-ray source using the HEAO-1 satellite during 1977–78. The Einstein Observatory was then used in 1981 to more precisely position the source, which was designated E 2003+225.[1] In 1982, J. A. Nousek and associates observed the optical counterpart and found it varied in brightness with a period of 3.706 hours, displaying strong emission lines of hydrogen and helium. They identified it as a variable of the AM Herculis type.[10] The system shows a brightness variation of 0.7 magnitude during each orbit, plus a short-term flickering of 0.2 magnitudes.[1]

The accepted model for this class of variable is a binary system with a red dwarf secondary in a close orbit with a magnetic white dwarf. The red dwarf is overflowing its Roche lobe and matter is streaming onto the white dwarf.[11] The magnetic field of the white dwarf draws this material toward the magnetic poles, and the material is heated to a sufficient temperature to emit X-rays.[12] In 1985, a weak, extended radio source was detected at the location of this system, suggesting it may be a remnant of a past nova event.[13] X-ray observations in 1991 suggested there are separate regions of hard and soft X-ray emission, indicating matter is being accreted along two poles. The soft X-ray site is likely at the magnetic pole furthest from the secondary star.[12]

The strength of the magnetic field in the white dwarf is estimated at ~30 MG. Over long periods, the system has been shown to switch between states of high and low brightness.[8] K. Mukai and associates in 1986 suggested that the primary dip in the light curve is due to the geometry of the system in combination with a partial eclipse of the primary accretion region by the accretion column. The secondary dip may be caused by the limb of the white dwarf partially eclipsing the active accretion region. The rotation period of the white dwarf appears to be locked to the orbital period.[8]

References

  1. ↑ 1.0 1.1 1.2 Nousek, J. A. et al. (February 1984), "E 2003+225 : a 3h42m AM Herculis type binary system.", Astrophysical Journal 277: 682–691, doi:10.1086/161739, Bibcode: 1984ApJ...277..682N. 
  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 Zacharias, N. et al. (February 2013), "The Fourth US Naval Observatory CCD Astrograph Catalog (UCAC4)", The Astronomical Journal 145 (2): 44, doi:10.1088/0004-6256/145/2/44, Bibcode: 2013AJ....145...44Z. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 Catalán, M. S. et al. (November 1999), "Mapping the secondary star in QQ Vulpeculae", Monthly Notices of the Royal Astronomical Society 310 (1): 123–145, doi:10.1046/j.1365-8711.1999.02972.x, Bibcode: 1999MNRAS.310..123C, http://sro.sussex.ac.uk/id/eprint/18737/1/MNRAS-1999-Catal%C3%A1n-123-45.pdf. 
  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. ↑ Osborne, J. P. et al. (August 1986), "A multi-wavelength study of the long-period AM Her system E2003+225 -I. The soft X-ray light curve and overall energy spectrum", Monthly Notices of the Royal Astronomical Society 221 (4): 823–838, doi:10.1093/mnras/221.4.823, Bibcode: 1986MNRAS.221..823O. 
  7. ↑ 7.0 7.1 7.2 Watson, C. A. et al. (May 2003), "Roche tomography of cataclysmic variables - II. Images of the secondary stars in AM Her, QQ Vul, IP Peg and HU Aqr", Monthly Notices of the Royal Astronomical Society 341 (1): 129–142, doi:10.1046/j.1365-8711.2003.06381.x, Bibcode: 2003MNRAS.341..129W. 
  8. ↑ 8.0 8.1 8.2 Halevin, A. V. et al. (October 2002), "Unstable processes in magnetic cataclysmic variables. I. Case of the long-period polar QQ Vulpeculae", Astronomy and Astrophysics 394: 171–179, doi:10.1051/0004-6361:20021107, Bibcode: 2002A&A...394..171H. 
  9. ↑ "QQ Vul". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=QQ+Vul. 
  10. ↑ Nousek, J. et al. (October 1982), Marsden, B. G., ed., "E2003+225", IAU Circular 3733: p. 2, Bibcode: 1982IAUC.3733....2N. 
  11. ↑ Mukai, K. et al. (February 1985), "X-Ray Optical and Ultraviolet Observations of the AM-Herculis System E2003+225", Space Science Reviews 40 (1–2): 151–155, doi:10.1007/BF00212879, Bibcode: 1985SSRv...40..151M, https://dare.uva.nl/personal/pure/en/publications/xray-optical-and-uv-observations-of-the-am-her-system-e2003--225(aeff6663-746c-48a9-a66c-97e34b6b88b3).html. 
  12. ↑ 12.0 12.1 Beardmore, A. P. et al. (April 1995), "ROSAT and GINGA observations of the magnetic cataclysmic variable QQ Vul: evidence for two-pole accretion", Monthly Notices of the Royal Astronomical Society 273 (3): 742–750, doi:10.1093/mnras/273.3.742, Bibcode: 1995MNRAS.273..742B. 
  13. ↑ Takalo, L. O.; Nousek, J. A. (June 1985), "E2000+223: a newly discovered old nova?", Publications of the Astronomical Society of the Pacific 97: 570–574, doi:10.1086/131569, Bibcode: 1985PASP...97..570T. 

Further reading

  • Sanad, M. R. (December 2010), "Spectral behavior of AM Her and QQ Vul in high and intermediate states in the UV", Astrophysics and Space Science 330 (2): 337–345, doi:10.1007/s10509-010-0403-1, Bibcode: 2010Ap&SS.330..337S. 
  • Staude, A. et al. (December 2004), Vrielmann, Sonja; Cropper, Mark, eds., "Tomography of AM Her and QQ Vul", Magnetic Cataclysmic Variables, IAU Colloquium 190, Proceedings of the Conference held 8-13 December, 2002 in Cape Town, South Africa, ASP Conference Proceedings (San Francisco: Astronomical Society of the Pacific) 315: p. 251, Bibcode: 2004ASPC..315..251S. 
  • Kafka, S.; Honeycutt, R. K. (April 2003), "The Puzzling Optical Light Curve of the Polar QQ Vulpeculae", The Astronomical Journal 125 (4): 2188–2195, doi:10.1086/368143, Bibcode: 2003AJ....125.2188K. 
  • Romero-Colmenero, E. et al. (March 2003), "Multi-epoch spectroscopy, polarimetry and photometry of the polar UW Pic", Monthly Notices of the Royal Astronomical Society 339 (3): 685–694, doi:10.1046/j.1365-8711.2003.06209.x, Bibcode: 2003MNRAS.339..685R. 
  • Kafka, S.; Honeycutt, R. K. (March 2003), Sterken, C., ed., "QQ Vul: variable features in the orbital light curve", Interplay of Periodic, Cyclic and Stochastic Variability in Selected Areas of the H-R Diagram, ASP Conference Series 292 (San Francisco: Astronomical Society of the Pacific) 292: p. 319, Bibcode: 2003ASPC..292..319K. 
  • Halevin, A. V. et al. (January 2002), Gänsicke, B. T.; Beuermann, K.; Reinsch, K., eds., "Accretion instabilities with time-scales from seconds to years in magnetic cataclysmic variables", The Physics of Cataclysmic Variables and Related Objects, ASP Conference Proceedings (San Francisco: Astronomical Society of the Pacific) 261: 155, ISBN 1-58381-101-X, Bibcode: 2002ASPC..261..155H. 
  • Schwope, Axel D. et al. (April 2000), "Multi-epoch Doppler tomography and polarimetry of QQ Vul", Monthly Notices of the Royal Astronomical Society 313 (3): 533–546, doi:10.1046/j.1365-8711.2000.03240.x, Bibcode: 2000MNRAS.313..533S. 
  • Belle, Kunegunda E. et al. (March 2000), "EUVE Observations of the Magnetic Cataclysmic Variable QQ Vulpeculae", The Publications of the Astronomical Society of the Pacific 112 (769): 343–348, doi:10.1086/316536, Bibcode: 2000PASP..112..343B. 
  • Cropper, Mark (April 1998), "Polarimetry of QQ Vul", Monthly Notices of the Royal Astronomical Society 295 (2): 353–359, doi:10.1046/j.1365-8711.1998.01333.x, Bibcode: 1998MNRAS.295..353C. 
  • Catalan, M. S. et al. (1996), Evans, A.; Wood, Janet H., eds., "QQ Vul Revisited", Cataclysmic variables and related objects. Astrophysics and Space Science Library; Proceedings of the 158th colloquium of the International Astronomical Union (IAU); held at Keele; United Kingdom; June 26-30; 1995, Astrophysics and Space Science Library (Dordrecht: Kluwer Academic Publishers) 208: p. 227, doi:10.1007/978-94-009-0325-8_69, ISBN 978-94-010-6632-7, Bibcode: 1996ASSL..208..227C. 
  • Mukai, K. et al. (April 1988), "An apparent visual companion of QQ Vul (E 2003+225)", Astronomy and Astrophysics 194: 153–156, Bibcode: 1988A&A...194..153M. 
  • Osborne, Julian P. et al. (April 1987), "A New Soft X-Ray Mode in the AM Herculis Object E2003+225", Astrophysical Journal Letters 315: L123, doi:10.1086/184873, Bibcode: 1987ApJ...315L.123O. 
  • Andronov, I. L.; Fuhrmann, B. (January 1987), "On the Period of QQ Vulpeculae: New Minima from Old Plates", Information Bulletin on Variable Stars 2976: 1, Bibcode: 1987IBVS.2976....1A. 
  • McCarthy, Patrick et al. (December 1986), "Time-resolved Spectrophotometry of the AM Herculis System E2003+225", Astrophysical Journal 311: 873, doi:10.1086/164825, Bibcode: 1986ApJ...311..873M. 
  • Mukai, K. et al. (August 1986), "A multi-wavelength study of the long-period AM Her system E2003+225 -II. Changes in the accretion geometry.", Monthly Notices of the Royal Astronomical Society 221 (4): 839–856, doi:10.1093/mnras/221.4.839, Bibcode: 1986MNRAS.221..839M. 
  • McCarthy, P. J. et al. (March 1985), "Time Resolved Spectrophotometry of the AM HER System E2003+225", Bulletin of the American Astronomical Society 17: 589, Bibcode: 1985BAAS...17..589M. 
  • Andronov, I. L.; Yavorskij, Yu. B. (October 1983), "Photometric study of AM Herculis-type star E 2003+225", Soviet Astronomy Letters 9: 291–292, Bibcode: 1983PAZh....9..556A. 




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