A common origin of magnetism from planets to white dwarfs

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hdl:2117/104213
Document typeArticle
Defense date2017-02-20
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ProjectDESARROLLO Y EXPLOTACION DE LA MISION LISA PATHFINDER Y CONTRIBUCIONES AL UNIVERSO GRAVITATORIO Y STE-QUEST (MINECO-ESP2013-47637-P)
EXPLOSIONES ESTELARES Y SUS ESCENARIOS EN ALTAS ENERGIAS: MODELOS, OBSERVACIONES Y TECNOLOGIA (MINECO-ESP2015-66134-R)
SIMULACIONES MULTIDIMENSIONALES DE NOVAS Y SUPERNOVAS IA (MINECO-AYA2014-59084-P)
SIMULACIONES MULTIDIMENSIONALES DE NOVAS Y SUPERNOVAS IA (MINECO-AYA2014-59084-P)
EXPLOSIONES ESTELARES Y SUS ESCENARIOS EN ALTAS ENERGIAS: MODELOS, OBSERVACIONES Y TECNOLOGIA (MINECO-ESP2015-66134-R)
SIMULACIONES MULTIDIMENSIONALES DE NOVAS Y SUPERNOVAS IA (MINECO-AYA2014-59084-P)
SIMULACIONES MULTIDIMENSIONALES DE NOVAS Y SUPERNOVAS IA (MINECO-AYA2014-59084-P)
Abstract
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, 12C and 16O, 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.
CitationIsern, J., Garcia-berro, E., Kulebi, B., Loren, P. A common origin of magnetism from planets to white dwarfs. "Astrophysical Journal Letters", 20 Febrer 2017, vol. 836, núm. L28, p. 1-5.
ISSN2041-8213
Publisher versionhttp://iopscience.iop.org/article/10.3847/2041-8213/aa5eae
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