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

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.[8] 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.[9] The system shows a brightness variation of 0.7 magnitude during each orbit, plus a short-term flickering of 0.2 magnitudes.[8]

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.[10] 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.[11] 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.[12] 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.[11]

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.[13] 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.[13]

References

  1. ^ a b c d e Brown, 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 at VizieR.
  2. ^ a b Zacharias, N.; et al. (February 2013), "The Fourth US Naval Observatory CCD Astrograph Catalog (UCAC4)", The Astronomical Journal, 145 (2): 44, arXiv:1212.6182, Bibcode:2013AJ....145...44Z, doi:10.1088/0004-6256/145/2/44, S2CID 119299381.
  3. ^ a b c d e 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, Bibcode:1999MNRAS.310..123C, doi:10.1046/j.1365-8711.1999.02972.x.
  4. ^ a b Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869.
  5. ^ 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: 823–838, Bibcode:1986MNRAS.221..823O, doi:10.1093/mnras/221.4.823.
  6. ^ a b c 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 Notice of the Royal Astronomical Society, 341 (1): 129–142, arXiv:astro-ph/0302115, Bibcode:2003MNRAS.341..129W, doi:10.1046/j.1365-8711.2003.06381.x.
  7. ^ "QQ Vul". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2022-09-02.
  8. ^ a b Nousek, J. A.; et al. (February 1984), "E 2003+225 : a 3h42m AM Herculis type binary system.", Astrophysical Journal, 277: 682–691, Bibcode:1984ApJ...277..682N, doi:10.1086/161739.
  9. ^ Nousek, J.; et al. (October 1982), Marsden, B. G. (ed.), "E2003+225", IAU Circular, vol. 3733, p. 2, Bibcode:1982IAUC.3733....2N.
  10. ^ 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, Bibcode:1985SSRv...40..151M, doi:10.1007/BF00212879.
  11. ^ a b 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, Bibcode:1995MNRAS.273..742B, doi:10.1093/mnras/273.3.742.
  12. ^ 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, Bibcode:1985PASP...97..570T, doi:10.1086/131569.
  13. ^ a b 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, Bibcode:2002A&A...394..171H, doi:10.1051/0004-6361:20021107.

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, Bibcode:2010Ap&SS.330..337S, doi:10.1007/s10509-010-0403-1.
  • 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, vol. 315, San Francisco: Astronomical Society of the Pacific, 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, Bibcode:2003AJ....125.2188K, doi:10.1086/368143.
  • Romero-Colmenero, E.; et al. (March 2003), "Multi-epoch spectroscopy, polarimetry and photometry of the polar UW Pic", Monthly Notice of the Royal Astronomical Society, 339 (3): 685–694, Bibcode:2003MNRAS.339..685R, doi:10.1046/j.1365-8711.2003.06209.x.
  • 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, p. 319, Bibcode:2003ASPC..292..319K.
  • Halevin, A. V.; et al. (January 2002), Gänsicke, B. T.; et al. (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, vol. 261, San Francisco: Astronomical Society of the Pacific, p. 155, Bibcode:2002ASPC..261..155H, ISBN 1-58381-101-X.
  • 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, arXiv:astro-ph/9911141, Bibcode:2000MNRAS.313..533S, doi:10.1046/j.1365-8711.2000.03240.x.
  • 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, vol. 112, no. 769, pp. 343–348, arXiv:astro-ph/9911529, Bibcode:2000PASP..112..343B, doi:10.1086/316536.
  • Cropper, Mark (April 1998), "Polarimetry of QQ Vul", Monthly Notices of the Royal Astronomical Society, 295 (2): 353–359, Bibcode:1998MNRAS.295..353C, doi:10.1046/j.1365-8711.1998.01333.x.
  • 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, Dordrecht: Kluwer Academic Publishers, p. 227, Bibcode:1996ASSL..208..227C, doi:10.1007/978-94-009-0325-8_69.
  • 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, Bibcode:1987ApJ...315L.123O, doi:10.1086/184873.
  • Andronov, I. L.; Fuhrmann, B. (January 1987), "On the Period of QQ Vulpeculae: New Minima from Old Plates", Information Bulletin on Variable Stars, vol. 2976, p. 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, Bibcode:1986ApJ...311..873M, doi:10.1086/164825.
  • 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: 839–856, Bibcode:1986MNRAS.221..839M, doi:10.1093/mnras/221.4.839.
  • 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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