Turbulent Diffusion of Magnetic Field Lines in the Heliosphere
Due to solar wind turbulence, Parker spirals are stochastic. The dispersion of magnetic field lines is described by a convection–diffusion equation for the field line density distribution, which is a function of the two heliographic angles in addition to the radial distance. Taking into account the...
Furkejuvvon:
| Váldodahkkit: | , , , , |
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| Materiálatiipa: | Artigo |
| Giella: | Inglês |
| Almmustuhtton: |
IOP Publishing
2026-01-01
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| Ráidu: | The Astrophysical Journal |
| Fáttát: | |
| Liŋkkat: | https://doi.org/10.3847/1538-4357/ae7a4f |
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