Abstract:
:The origin of highly magnetized white dwarfs has remained a mystery since their initial discovery. Recent observations indicate that the formation of high-field magnetic white dwarfs is intimately related to strong binary interactions during post-main-sequence phases of stellar evolution. If a low-mass companion, such as a planet, brown dwarf, or low-mass star, is engulfed by a post-main-sequence giant, gravitational torques in the envelope of the giant lead to a reduction of the companion's orbit. Sufficiently low-mass companions in-spiral until they are shredded by the strong gravitational tides near the white dwarf core. Subsequent formation of a super-Eddington accretion disk from the disrupted companion inside a common envelope can dramatically amplify magnetic fields via a dynamo. Here, we show that these disk-generated fields are sufficiently strong to explain the observed range of magnetic field strengths for isolated, high-field magnetic white dwarfs. A higher-mass binary analogue may also contribute to the origin of magnetar fields.
journal_name
Proc Natl Acad Sci U S Aauthors
Nordhaus J,Wellons S,Spiegel DS,Metzger BD,Blackman EGdoi
10.1073/pnas.1015005108subject
Has Abstractpub_date
2011-02-22 00:00:00pages
3135-40issue
8eissn
0027-8424issn
1091-6490pii
1015005108journal_volume
108pub_type
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