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On the origin of magnetic fields in stars

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Wurster_2018_On_the_origin_MNRAS_2450.pdf (4.359Mb)
Date
12/2018
Author
Wurster, J.
Bate, Matthew R.
Price, Daniel J.
Keywords
Magnetic fields
MHD
Methods: numerical
Stars: formation
QA75 Electronic computers. Computer science
QB Astronomy
QC Physics
DAS
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Abstract
Are the kG-strength magnetic fields observed in young stars a fossil field left over from their formation or are they generated by a dynamo? We use radiation non-ideal magnetohydrodynamics simulations of the gravitational collapse of a rotating, magnetized molecular cloud core over 17 orders of magnitude in density, past the first hydrostatic core to the formation of the second, stellar core, to examine the fossil field hypothesis. Whereas in previous work, we found that magnetic fields in excess of 10 kG can be implanted in stars at birth, this assumed ideal magnetohydrodynamics (MHD), i.e. that the gas is coupled to the magnetic field. Here we present non-ideal MHD calculations which include Ohmic resistivity, ambipolar diffusion, and the Hall effect. For realistic cosmic ray ionization rates, we find that magnetic field strengths of ≲ kG are implanted in the stellar core at birth, ruling out a strong fossil field. While these results remain sensitive to resolution, they cautiously provide evidence against a fossil field origin for stellar magnetic fields, suggesting instead that magnetic fields in stars originate in a dynamo process.
Citation
Wurster , J , Bate , M R & Price , D J 2018 , ' On the origin of magnetic fields in stars ' , Monthly Notices of the Royal Astronomical Society , vol. 481 , no. 2 , pp. 2450-2457 . https://doi.org/10.1093/mnras/sty2438
Publication
Monthly Notices of the Royal Astronomical Society
Status
Peer reviewed
DOI
https://doi.org/10.1093/mnras/sty2438
ISSN
0035-8711
Type
Journal article
Rights
© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/sty2438
Collections
  • University of St Andrews Research
URL
https://arxiv.org/abs/1809.01234
URI
http://hdl.handle.net/10023/18768

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