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Cosmic ray interactions in the solar atmosphere

Hudson, Hugh S.; MacKinnon, Alec; Szydlarski, Mikolaj Marcin; Carlsson, Mats
Journal article; PublishedVersion; Peer reviewed
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stz3373.pdf (2.983Mb)
Year
2019
Permanent link
http://urn.nb.no/URN:NBN:no-78380

CRIStin
1767009

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Appears in the following Collection
  • Institutt for teoretisk astrofysikk [690]
  • CRIStin høstingsarkiv [15189]
Original version
Monthly notices of the Royal Astronomical Society. 2019, 491 (4), 4852-4856, DOI: https://doi.org/10.1093/mnras/stz3373
Abstract
High-energy particles enter the solar atmosphere from Galactic or solar coronal sources, and produce ‘albedo’ emission from the quiet Sun that is now observable across a wide range of photon energies. The interaction of high-energy particles in a stellar atmosphere depends essentially upon the joint variation of the magnetic field and plasma density, which heretofore has been characterized parametrically as P ∝ Bα with P the gas pressure and B the magnitude of the magnetic field. We re-examine that parametrization by using a self-consistent 3D MHD model (Bifrost) and show that this relationship tends to P ∝ B3.5 ± 0.1 based on the visible portions of the sample of open-field flux tubes in such a model, but with large variations from point to point. This scatter corresponds to the strong meandering of the open-field flux tubes in the lower atmosphere, which will have a strong effect on the prediction of the emission anisotropy (limb brightening). The simulations show that much of the open flux in coronal holes originates in weak-field regions within the granular pattern of the convective motions seen in the simulations.
 
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