White dwarf rotation and the shapes of nova remnants

Details White dwarf rotation and the shapes of nova remnants White dwarf rotation and the shapes of nova remnants

Jul 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...239..253f&link_type=abstract

Astrophysical Journal, Part 1, vol. 239, July 1, 1980, p. 253-256.

Astronomy and Astrophysics

Astrophysics

7

Stellar Envelopes, Stellar Rotation, Supernova Remnants, White Dwarf Stars, Angular Momentum, Main Sequence Stars, Shapes, Stellar Mass Ejection, Stellar Models

Scientific paper

The elongated appearance of many nova remnants is explained due to rapid rotation of the parent white dwarf. The principal influence of this rotation is seen to be the spin angular momentum given to material ejected in the equatorial directions. Resulting shells should be oblate. Implied white dwarf rotation periods are of the order of minutes, consistent with that apparently observed for DQ Herculis (N Her 1934) and V533 Herculis (N Her 1963).

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