Classical novae as fast magnetic rotators

Details Classical novae as fast magnetic rotators Classical novae as fast magnetic rotators

Apr 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...257..548o&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 257, no. 2, p. 548-556.

Astronomy and Astrophysics

Astronomy

18

Magnetic Stars, Novae, Stellar Magnetic Fields, Stellar Models, Stellar Rotation, Stellar Winds, Magnetohydrodynamics, Stellar Evolution, Stellar Mass Ejection, Ultraviolet Astronomy, White Dwarf Stars, X Ray Astronomy

Scientific paper

UV and X-ray observations of classical novae after the outburst suggest a short turn-off time scale, of the order of a few years. This is reconciled with the postnova nuclear burning stage of the remaining envelope only if the nova white dwarfs are very massive. We examine this issue considering that a relevant number of systems that undergo classical nova outburst can be intermediate polars and AM Her type, implying that they have sufficiently strong magnetic fields and high rotation rates to be fast magnetic rotators. We compare approximate postnova magnetic wind solutions with the optically thick winds studied by Kato in a series of papers from 1983 to 1989. The relationship of the envelope mass to the mass-loss rate changes for rotating white dwarfs with magnetic fields of the order of a few million Gauss; the mass loss phase is shorter than in the case of low magnetic field and less envelope mass is left on the white dwarf at the end. Intermediate polars nova systems can enter the regime of centrifugal magnetic rotators in which the whole envelope can be ejected no matter under which conditions the thermonuclear runaway occurred. We can thus reconcile the models with the observations without having to resort to very high white dwarf masses in classical novae.

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