Christopher Thompson's research while affiliated with University of Toronto and other places
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Publications (3)
The internal rotation and magnetism of evolved massive stars are considered in response to i) the inward pumping of angular momentum through deep and slowly rotating convective layers; and ii) the winding up of a helical magnetic field in radiative layers. Field winding can transport angular momentum effectively even when the toroidal field is limi...
The internal rotation of post-main sequence stars is investigated, in
response to the convective pumping of angular momentum toward the stellar core,
combined with a tight magnetic coupling between core and envelope. The spin
evolution is calculated using model stars of initial mass 1, 1.5 and
$5\,M_\odot$, taking into account mass loss on the gian...
The magnetism and rotation of white dwarf (WD) stars are investigated in
relation to a hydromagnetic dynamo operating in the progenitor during shell
burning phases. We find that the downward pumping of angular momentum in the
convective envelope can, by itself, trigger dynamo action near the
core-envelope boundary in an isolated intermediate-mass s...
Citations
... Further advances in this field concern dynamo models that differ more substantially from MRI or Tayler-instability driven ones. In these pictures, the magnetic field is typically derived from the induction equation, and the field generation is attributed to differential rotation via the velocity field of the fluid in a mean-field dynamo [156,[189][190][191][192][193]. ...
Reference: Review: Magnetism in High-Mass Stars
... One of the key developments was the recognition that magnetic white dwarfs are nearly exclusively found as isolated stars, or in cataclysmic variables (Liebert et al. 2005). This empirical finding led to the hypothesis that fields are generated during common envelope evolution (Tout et al. 2008;Nordhaus et al. 2011;Belloni & Schreiber 2020), a process that may function effectively for stars, brown dwarfs, and giant planets that are engulfed during the post-main sequence (Farihi et al. 2011;Kissin & Thompson Farihi et al. where the principal findings can be summarized as follows. ...
... MNRAS 521, 4122-4130 (2023) made on angular momentum transport mechanisms through more precise measures of the core-to-surface rotation ratios of post-MS stars (Deheuvels et al. 2014 ), and of the position and strength of a rotation rate gradient (Di Mauro et al. 2018 ). For example, a rotation profile with a constant rotation rate internal to the base of the conv ectiv e zone (BCZ), and a decreased rotation rate that is inversely dependent on radius in the BCZ, could be indicative of angular momentum transport from deep fossil magnetic fields (Gough & Thompson 1990 ;Kissin & Thompson 2015 ;Takahashi & Langer 2021 ). This results from differential rotation being damped along poloidal field lines (Garaud 2002 ;Strugarek, Brun & Zahn 2011 ). ...
