Effect of solar corona conditions on flare particle propagation

✍ Scribed by G. Cherki; J. P. Mercier; A. Raviart; L. Treguer; D. Maccagni; F. Perotti; G. Villa

• Publisher: Springer
• Year: 1974
• Tongue: English
• Weight: 338 KB
• Volume: 34
• Category: Article
• ISSN: 0038-0938
• DOI: 10.1007/bf00149615

✦ Synopsis

Data on high energy electrons and protons in different energy windows are analyzed and compared for two solar flares which occurred at 37 W solar longitude on the 25th February 1969 and the 29th March 1970. While the data for the first of these flares can be interpreted in the framework of a diffusion model with suitable values of the parallel diffusion coefficient, in order fo explain the time behaviour of the different particles after the second event, we are led to suppose that the coronal magnetic fields are such that particles of different rigidity are ejected at different longitudes and that there is no good magnetic connection of the Earth with the flare region. * Called 'classical' in Dilworth et al. (1972).