Nonlocal heat transport in the solar wind
It is shown that a nonlocal, suprathermal tail originated near the solar corona base dominates the conductive energy flux at distances r ≥: 2 R ⊙ . A nonlocal analytical expression for the electron heat flux in weakly collisional plasmas is derived by solving the Fokker-Planck equation...
Guardado en:
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1996
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| Acceso en línea: | https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v462_n2PARTI_p1005_Canullo http://hdl.handle.net/20.500.12110/paper_0004637X_v462_n2PARTI_p1005_Canullo |
| Aporte de: |
| Sumario: | It is shown that a nonlocal, suprathermal tail originated near the solar corona base dominates the conductive energy flux at distances r ≥: 2 R ⊙ . A nonlocal analytical expression for the electron heat flux in weakly collisional plasmas is derived by solving the Fokker-Planck equation in a narrow, tail energy range. A correction to the anisotropy of the distribution function due to the divergent magnetic field lines was included. This term is essential to recover from the delocalization prescription, in the limit r ≥ 6 R ⊙ , the well-known Hollweg's Ansatz for the "collisionless" heat flux. In the intermediate region 2 R ȯ r ≤ 6 R ⊙ , the nonlocal convolution smoothly interpolates between the classical Spitzer-Härm's formula and the so-called collisionless régime. © 1996. The American Astronomical Society. All rights reserved. |
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