Abstract / Description of output
Interplanetary shocks can accelerate both solar wind ions and
flare-released high-energy particles to high energies. The acceleration
process is generally thought to be diffusive shock acceleration although
almost entirely based on a highly simplified steady-state description.
The importance of the evolving shock and the time constraints for
accelerating particles diffusively at a shock, coupled to the
inhomogeneous magnetic field and the expanding solar wind have not been
widely recognized. We have developed recently a fully time-dependent
model to describe particle acceleration at an expanding interplanetary
shock wave, including the self-consistent calculation of the spatial
diffusion coefficient in the vicinity of the shock, particle escape and
transport into the upstream wind. We review results for strong and weak
interplanetary shocks, showing intensity profiles, escaping particle
spectra at 1 AU, spectra at and behind the shock, particle
distributions, and estimate the maximum possible energies that can be
accelerated at an interplanetary shock. Preliminary results for 2D
time-dependent interplanetary shocks are presented too.
Original language | English |
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Pages | 4 |
Publication status | Published - 1 Dec 2002 |
Event | American Geophysical Union, Fall Meeting 2002 - , United Kingdom Duration: 6 Dec 2002 → 10 Dec 2002 |
Conference
Conference | American Geophysical Union, Fall Meeting 2002 |
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Country/Territory | United Kingdom |
Period | 6/12/02 → 10/12/02 |
Keywords / Materials (for Non-textual outputs)
- 2111 Ejecta
- driver gases
- and magnetic clouds
- 2114 Energetic particles
- heliospheric (7514)
- 2134 Interplanetary magnetic fields
- 2139 Interplanetary shocks