摘要:

We consider the transport of protons in a spatially‐bounded magnetized plasma containing a homogeneous distribution of Alfve´n wave turbulence. The protons interact strongly with the waves via cyclotron resonance, and are in turn pitch‐angle scattered and spatially diffused throughout the plasma. Upon traversing one of the boundaries, a proton escapes from the region. We solve numerically the diffusion equation describing this process for the number of trapped particles as a function of time. We find that a leaky‐box approximation is in poor agreement with the exact result when the turbulence injection rate is small, which is likely the prevailing condition after particle acceleration and during subsequent transport. On the other hand, this approximation nevertheless yields acceptable results when used in acceleration models. ©1996 American Institute of Physics.

ISSN:0094-243X    

DOI:10.1063/1.50986

出版商:AIP    

年代:1996

数据来源: AIP

摘要:

This paper is a summary of the presentations on X‐ray observations and electron acceleration mechanisms at the workshop. The emphasis is on dispelling myths, starting with the originalSolar Flare Mythand including others, both serious and not so serious. ©1996 American Institute of Physics.

ISSN:0094-243X    

DOI:10.1063/1.50987

出版商:AIP    

年代:1996

数据来源: AIP

摘要:

Solar flares provide a unique site for the study of energy release and particle acceleration in astrophysics. This paper summarizes the charged particle and gamma ray aspects of the Workshop on High Energy Solar Physics held at the Goddard Space Flight Center in August 1995. The X‐ray aspects of the Workshop are summarized in another paper. Here are our highlights: (i) both the charged particle, and now also gamma ray observations have shown that stochastic acceleration due to gyroresonant interactions with plasma waves is very important in solar flares; (ii) CME driven shocks accelerate the particles observed in space from gradual flares; (iii) accelerated MeV/nucl ions can contain a large fraction of the energy released in flares; (iv) GeV ions are either trapped at the Sun or accelerated for hours; (v) nuclear gamma ray spectroscopy has become a tool for abundance determinations in the solar atmosphere; (vi) behind‐the‐limb flares can provide imaging information for solar gamma ray emission. ©1996 American Institute of Physics.

ISSN:0094-243X    

DOI:10.1063/1.50988

出版商:AIP    

年代:1996

数据来源: AIP