Iphigenia in Aulis

Cumming, Julie E.

doi:10.1093/gmo/9781561592630.article.o003405

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The Stellar Dynamo1

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2017

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“…Furthermore, the characteristic Ohmic decay time τ Ω ∼ R 2 WD /η ≃ 10 18 s is much longer than the age of the white dwarf. Consequently, once the magnetic field is generated, it will remain almost constant for long times (Cumming 2002).…”

Section: The Stellar Dynamomentioning

confidence: 99%

A Common Origin of Magnetism from Planets to White Dwarfs

Isern

Garcı́a–Berro

Külebi

et al. 2017

ApJL

111

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Isolated magnetic white dwarfs have field strengths ranging from kilogauss to gigagauss. However, the origin of the magnetic field has not been hitherto elucidated. Whether these fields are fossil, hence the remnants of original weak magnetic fields amplified during the course of the evolution of their progenitor stars, or are the result of binary interactions, or, finally, they are produced by other internal physical mechanisms during the cooling of the white dwarf itself, remains a mystery. At sufficiently low temperatures, white dwarfs crystallize. Upon solidification, phase separation of its main constituents, 12 C and 16 O, and of the impurities left by previous evolution occurs. This process leads to the formation of a Rayleigh-Taylor unstable liquid mantle on top of a solid core. This convective region, as it occurs in solar system planets like the Earth and Jupiter, can produce a dynamo able to yield magnetic fields of strengths of up to 0.1 MG, thus providing a mechanism that could explain magnetism in single white dwarfs.

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Section: The Stellar Dynamomentioning

confidence: 99%