Abstract
| Language | English |
|---|---|
| Pages | 329-335 |
| Number of pages | 7 |
| Journal | Solar Physics |
| Volume | 147 |
| Issue number | 2 |
| DOIs | |
| Publication status | Published - 1 Oct 1993 |
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Keywords
- accelerated protons
- solar flares
- spectral index
- resonance
- MHD turbulence
- electron acceleration
- proton acceleration
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Proton acceleration in flares and magnetohydrodynamic solar activity. / Tsytovich, V. N.; Bingham, R.; Angelis, U. de; Bryant, D. A.; Nairn, C. M. C.
In: Solar Physics, Vol. 147, No. 2, 01.10.1993, p. 329-335.Research output: Contribution to journal › Article
TY - JOUR
T1 - Proton acceleration in flares and magnetohydrodynamic solar activity
AU - Tsytovich, V. N.
AU - Bingham, R.
AU - Angelis, U. de
AU - Bryant, D. A.
AU - Nairn, C. M. C.
PY - 1993/10/1
Y1 - 1993/10/1
N2 - The possibility of accelerated protons in solar flares having a sharp change in their spectral index is discussed. The analysis is based on the Tsytovich (1982, 1984, 1987a, b, c) acceleration model by MHD turbulence, which is shown to have different resonant conditions for non-relativistic and relativistic particles. The different resonant condition is shown to result in a sharp change in the accelerated proton spectral index, even in the absence of any peculiarity in the spectra of the MHD turbulence. Time scales for accelerated protons to relativistic energies are also derived, and shown to be consistent with observations. We also show that the threshold energy for electron acceleration by low frequency MHD turbulence is much greater than for proton acceleration. The turbulence therefore preferentially accelerates protons.
AB - The possibility of accelerated protons in solar flares having a sharp change in their spectral index is discussed. The analysis is based on the Tsytovich (1982, 1984, 1987a, b, c) acceleration model by MHD turbulence, which is shown to have different resonant conditions for non-relativistic and relativistic particles. The different resonant condition is shown to result in a sharp change in the accelerated proton spectral index, even in the absence of any peculiarity in the spectra of the MHD turbulence. Time scales for accelerated protons to relativistic energies are also derived, and shown to be consistent with observations. We also show that the threshold energy for electron acceleration by low frequency MHD turbulence is much greater than for proton acceleration. The turbulence therefore preferentially accelerates protons.
KW - accelerated protons
KW - solar flares
KW - spectral index
KW - resonance
KW - MHD turbulence
KW - electron acceleration
KW - proton acceleration
UR - http://link.springer.com/journal/11207
U2 - 10.1007/BF00690722
DO - 10.1007/BF00690722
M3 - Article
VL - 147
SP - 329
EP - 335
JO - Solar Physics
T2 - Solar Physics
JF - Solar Physics
SN - 0038-0938
IS - 2
ER -