期刊
PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA
卷 108, 期 8, 页码 3135-3140出版社
NATL ACAD SCIENCES
DOI: 10.1073/pnas.1015005108
关键词
magnetohydrodynamics; compact objects
资金
- National Aeronautics and Space Administration (NASA) [HST-AR-12146, NNX07AG80G]
- Chandra X-Ray Center [PF9-00065, NAS8-03060]
- National Science Foundation [PHY-0903797, AST-0807363]
- Division Of Physics
- Direct For Mathematical & Physical Scien [903797] Funding Source: National Science Foundation
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.
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