Obliquity and magnetic dipole radiation from collapsing, rotating, magnetized stars

Details Obliquity and magnetic dipole radiation from collapsing, rotating, magnetized stars Obliquity and magnetic dipole radiation from collapsing, rotating, magnetized stars

Apr 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992ap%26ss.190..131c&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 190, no. 1, April 1992, p. 131-138.

Astronomy and Astrophysics

Astrophysics

Magnetic Dipoles, Magnetic Stars, Neutron Stars, Stellar Magnetic Fields, Stellar Rotation, White Dwarf Stars, Eccentricity, Stellar Evolution, Stellar Models, Stellar Radiation

Scientific paper

The evolution of a collapsing (or exploding), uniformly rotating, uniformly magnetized spheroidal star with nonaligned rotational and magnetic axes is considered. Analytical expressions were obtained for the change in angle (obliquity) between the two axes (based on the frozen field condition), and the energy loss via magnetic dipole radiation. Numerical estimates with typical data show that the obliquity increases with the collapse from white dwarf to neutron star, and the energy loss could be as much as 4 x 10 exp 39 ergs, about twice the amount emitted when the two axes are aligned.

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