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QQ Vul Revisited

Published online by Cambridge University Press:  12 April 2016

M.S. Catalán ,
S. D. Davey ,
R. C. Smith  and
D. H. P. Jones
M.S. Catalán
Affiliation:
Dept. of Physics and Astronomy, University of St Andrews, Fife KY16 9SS, UK Astronomy Centre, Division of Physics and Astronomy, University of Sussex, Brighton, BN1 9QH, UK
S. D. Davey
Affiliation:
Astronomy Centre, Division of Physics and Astronomy, University of Sussex, Brighton, BN1 9QH, UK
R. C. Smith
Affiliation:
Dept. of Physics and Astronomy, University of St Andrews, Fife KY16 9SS, UK
D. H. P. Jones
Affiliation:
RGO, Madingley Rd., Cambridge, CB3 0EZ, UK

Abstract

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With simultaneous blue (λλ4200–5000 Å) and far-red (λλ7950–8380 Å) phase-resolved, high resolution spectrophotometry, we re-examine the magnetic CV QQ Vul. A thorough radial velocity and flux analysis of all the observable features is carried out. We derive a complete set of system parameters and classify the donor star to be a spectral type M4.5 V. In addition to the Balmer, He I and He II emission lines in the blue range, arising from the accretion regions, we detect various emission features which solely follow the movement of the secondary star. The lines, which we interpret as reprocessed light from the illuminated hemisphere of the donor star, are Mg II at λ4481 Å, He II at λ8236 Å and C I at λ8335 Å. Intensity maps based on the line flux and radial velocity variations of the Na I absorption near λ8190 Å and Mg II emission feature were also made. These show that the line distribution on the surface of the donor is consistent with being symmetric. As a result of our analysis the position of the real zero phase was found to be at ϕ = 0.42 of the linear polarisation ephemeris.

Type
Polar Systems
Information
International Astronomical Union Colloquium , Volume 158: Cataclysmic Variables and Related Objects , 1996 , pp. 227 - 228
Copyright
Copyright © Kluwer 1996

References

Davey, S.C., Smith, R.S., 1992, MNRAS, 257, 476 CrossRefGoogle Scholar
Martin, J.S., Friend, M.T., Smith, R.C., et al., 1989, MNRAS, 240, 519 CrossRefGoogle Scholar
Mukai, K., Charles, P.A., 1987, MNRAS, 226, 209 CrossRefGoogle Scholar
Nousek, J.A., Takalo, L.O., Schmidt, G.D., et al., 1984, Ap. J., 277, 682 Google Scholar
Nugent, J.J., Jensen, K.A., Nousek, L.A., et al., 1983, Ap. J. Supp., 51, 1 CrossRefGoogle Scholar
Osborne, J.P., Beuermann, K., Charles, P., et al., 1987, Ap. J., 315, L123 Google Scholar
Wade, R.A., Horne, K., 1988, Ap. J., 324, 411 CrossRefGoogle Scholar