---
abstract: 'The solar wind wave heating models require substantial amount of wave
  power in order to efficiently heat and accelerate solar wind. The level of fluctuations
  is however limited by energetic particle observations. The simplest cyclotron sweep
  models result in convection-dominated transport, contradicting observations. However,
  models incorporating wave-wave -interactions, which cause wave energy to cascade
  in wavenumber, allow more reasonable energetic particle transport in the interplanetary
  space. The mean free path of the energetic particles remains still relatively short
  in the corona, providing favorable conditions for coronal mass ejection (CME) related
  shock acceleration. We study the consequences of this scenario on the energetic
  particle production related to CMEs. The role of self-generated waves is also discussed.'
adsnote: Provided by the SAO/NASA Astrophysics Data System
adsurl: https://ui.adsabs.harvard.edu/abs/2003AdSpR..32.2603L
authors:
- T. Laitinen
- R. Vainio
category: publications
date: '2003-01-01'
doi: 10.1016/S0273-1177(03)00932-3
draft: false
featured: false
journal: Advances in Space Research
month: January
number: '12'
pages: 2603-2608
projects: []
publication: Advances in Space Research
publication_types:
- '2'
tags: []
title: 'Shock acceleration of energetic particles in wave heated corona'
type: ARTICLE
volume: '32'
year: '2003'
---