Magnetic field evolution in white dwarfs

Details Magnetic field evolution in white dwarfs Magnetic field evolution in white dwarfs

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...313..284w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 313, Feb. 1, 1987, p. 284-297.

Astronomy and Astrophysics

Astrophysics

43

Carbon Stars, Stellar Evolution, Stellar Magnetic Fields, Stellar Models, White Dwarf Stars, Decay Rates, Electrical Resistivity, Magnetic Flux, Magnetohydrodynamic Flow, Time Dependence

Scientific paper

The authors have carried out detailed calculations of magnetic field decay in white dwarfs using an evolutionary sequence of 0.6 M_sun; carbon white dwarf models to solve the time-dependent MHD equation numerically. The models are radially symmetric and nonrotating. The magnetic field is purely poloidal. The central conductivity of the older models increases relatively quickly. As a result, the decay time scale also increases and in fact is always longer than the age of the star. In spite of this, a field consisting of an initially pure fundamental eigenmode decays appreciably (≡50% at the surface in 1010yr). This is because the evolving structure of the star changes the decay eigenmodes, so that the field becomes a mixture of higher order modes which decay more rapidly than the fundamental.

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