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Collapse of White Dwarfs in Close Binary Systems

Published online by Cambridge University Press:  12 April 2016

R. Canal  and
J. Isern
R. Canal
Affiliation:
Departamento de Fisica de la Tierra y del Cosmos, Universidad de Barcelona
J. Isern
Affiliation:
Departamento de Fisica de la Tierra y del Cosmos, Universidad de Barcelona

Extract

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The presence of neutron stars in close binary systems, shown by the pulsating X-ray sources, poses the problem of their origin. In the case of the low-mass (M1 + M2 ≤ 5 M⊙) X-ray binaries, the neutron star might have originated from a massive white dwarf, driven over the Chandrasekhar limit by mass transfer (Schatzman 1974). A similar scenario had been put forward by Whelan and Iben (1973) for type I supernovae. To solve the problem of the very low eccentricities observed for the orbits, and to facilitate keeping the system bound after neutron star formation, Canal and Schatzman (1976) suggested a non explosive collapse of the white dwarf to a neutron star. The occurence of this kind of collapse depended on the possibility of avoiding thermonuclear ignition by means of neutronization. Since there is a density interval where the electron captures on carbon go faster than the pycnonuclear reactions, just above the critical density for the beginning of the collapse, there seemed also to be a chance of escape from thermonuclear runaway. A closer examination of this picture leads, however, to significant changes.

Type
Colloquium Session I
Information
International Astronomical Union Colloquium , Volume 53: White Dwarfs and Variable Degenerate Stars , August 1979 , pp. 52 - 55
Copyright
Copyright © The University of Rochester 1979

References

Alastuey, A., and Jancovici, B. 1978, Ap.J., 226, 1034.CrossRefGoogle Scholar
Bruenn, S.W. 1972, Ap.J. Suppl., 24, 283.Google Scholar
Bruenn, S.W. 1973, Ap.J. Lett., 183, L125.CrossRefGoogle Scholar
Canal, R., and Schatzman, E. 1976, Astron. and Astrophys., 46, 229.Google Scholar
Chechetkin, V.M., Imshennik, V.S., Ivanova, L.N., and Nadyozhin, D.K. 1977, in Supernovae, ed. Schramm, D.N. (Reidel: Dordrecht), p.159.Google Scholar
Mazurek, T.J., Truran, J.W., and Cameron, A.G.W. 1974, Astrophys. and Space Sci., 27, 261.CrossRefGoogle Scholar
Mazurek, T.J., Meier, D.L., and Wheeler, J.C. 1977, Ap.J., 213, 518.Google Scholar
Nomoto, K., Sugimoto, D., and Neo, S. 1976, Astrophys. and Space Sci., 39, L37.Google Scholar
Ono, Y. 1960, Progr. Theor. Phys., Kyoto, 24, 825.Google Scholar
Salpeter, E.E., and Van Horn, H.M. 1969, Ap.J., 155, 183.Google Scholar
Saslaw, W. 1968, M.N.R.A.S., 138, 337.Google Scholar
Schatzman, E. 1974, in The Nuclei of Galaxies, Black Holes, and Collapsed Matter, Course III, Inter. School of Cosmology and Gravitation, Erice, Italy.Google Scholar
Schatzman, E. 1978, Astron. and Astrophys., 65, L17.Google Scholar
Whelan, J., and Iben, I. 1973, Ap.J., 186, 1007.CrossRefGoogle Scholar