Hostname: page-component-78c5997874-m6dg7 Total loading time: 0 Render date: 2024-11-02T22:49:12.423Z Has data issue: false hasContentIssue false
  • English
  • Français

Masses and Magnetic Fields of White Dwarfs in Cataclysmic Variables

Published online by Cambridge University Press:  12 April 2016

J.P. Lasota ,
J.M. Hameury  and
A.R. King
J.P. Lasota
Affiliation:
DARC, Observatoire de Paris, Section de Meudon, F-92195 Meudon Principal cédex, France
J.M. Hameury
Affiliation:
DAEC, Observatoire de Paris, Section de Meudon, F-92195 Meudon Principal cédex, andUniversité Paris 7, France
A.R. King
Affiliation:
DARC, Observatoire de Paris, Section de Meudon, F-92195 Meudon Principal cédex, France DAEC, Observatoire de Paris, Section de Meudon, F-92195 Meudon Principal cédex, andUniversité Paris 7, France Astronomy Department, University of Leicester, Leicester LE17RH, UK

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We show that the existence of the AM Her period spike implies (i) a unique white dwarf mass ≃ 0.6 − 0.7M⊙ for most magnetic CV’s (ii) nova explosions remove exactly the accreted mass from magnetic white dwarfs, and (iii) the maximum magnetic field for most CV’s is ≤ 4 × 107 G. The existence of the spike is very strong support for the idea that the period gap results from a drastic reduction of angular momentum losses when the secondary star becomes fully convective.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 114: White Dwarfs , 1989 , pp. 337 - 340
Copyright
Copyright © Springer-Verlag 1989

References

1. Morris, S.L., Schmidt, G.D., Liebert, J., Stocke, J., Gioia, I. & Maccacaro, T., 1987. Astrophys. J., 314, 641.CrossRefGoogle Scholar
2. Hameury, J.M., King, A.R., Lasota, J.P. & Ritter, H., 1988a. Mon. Not. R. astr. Soc., 231, 535.Google Scholar
3. Rappaport, S., Verbunt, F. & Joss, P.C., 1983. Astrophys. J., 275, 713.CrossRefGoogle Scholar
4. Spruit, H.C. & Ritter, H., 1983. Astr. Astrophys., 124, 267.Google Scholar
5. Hameury, J.M., King, A.R. & Lasota, J.P., 1988b. Astr. Astrophys., 195, L12.Google Scholar
6. Beuermann, K., Thomas, H.C. & Schwope, A., 1988. Astr. Astrophys., 195, L15.Google Scholar
7. Berriman, G. & Smith, P.S., 1988. Astrophys. J., 329, L97.CrossRefGoogle Scholar
8. Hameury, J.M., King, A.R., Lasota, J.P. & Livio, M., 1988c. Mon. Not. R. astr. Soc. submittedGoogle Scholar
9. Hameury, J.M., King, A.R. & Lasota, J.P., 1988d. Mon. Not. R. astr. Soc, submittedGoogle Scholar
10. King, A.R., Frank, J. & Ritter, H., 1985. Mon. Not. R. astr. Soc., 213, 185.Google Scholar
11. Hameury, J.M., King, A.R. & Lasota, J.P., 1986. Mon. Not. R. astr. Soc., 218, 695.Google Scholar
12. Warner, B., 1976. in Structure and evolution of close binary systems, IAU symposium No 73, eds. Eggleton, P., Mitton, S. and Whelan, J., Reidel, Dordrecht, Holland, p. 85.Google Scholar
13. Schmidt, G., Stockman, H.S. & Grandi, S.A., 1986. Astrophys. J., 300, 804.CrossRefGoogle Scholar
14. Schmidt, G., 1987. Mem. Soc. Astron. It. 209, 227.Google Scholar