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The heating of the thermal plasma with energetic electrons in small solar flares
| Content Provider | NASA Technical Reports Server (NTRS) |
|---|---|
| Author | Lin, R. P. Lin, H. A. |
| Copyright Year | 1986 |
| Description | The energetic electrons deduced from hard X-rays in the thick target model may be responsible for heating of soft X-ray plasma in solar flares. It is shown from OSO-7 studies that if a cutoff of 10 keV is assumed, the total electron is comparable to the thermal plasma energy. However, (1) the soft X-ray emission often appears to begin before the hard X-ray burst, (2) in about one-third of flares there is no detectable hard X-ray emission, and (3) for most events the energy content (assuming constant density) of soft X-ray plasma continues to rise after the end of the hard X-ray burst. To understand these problems we have analyzed the temporal relationship between soft X-rays and hard X-rays for 20 small events observed by ISEE-3 during 1980. One example is shown. The start of soft X-ray and hard X-ray bursts is defined as the time when the counting rates of the 4.8 to 5. keV and 25.8 to 43.2 keV channels, respectively, exceed the background by one standard deviation. |
| File Size | 141445 |
| Page Count | 4 |
| File Format | |
| Alternate Webpage(s) | http://archive.org/details/NASA_NTRS_Archive_19860015154 |
| Archival Resource Key | ark:/13960/t7qp1111v |
| Language | English |
| Publisher Date | 1986-04-01 |
| Access Restriction | Open |
| Subject Keyword | Solar Physics Solar X-rays Solar Flares Thermal Plasmas Oso-7 Electron Energy Plasma Heating Energetic Particles Electrons Ntrs Nasa Technical Reports Server (ntrs) Nasa Technical Reports Server Aerodynamics Aircraft Aerospace Engineering Aerospace Aeronautic Space Science |
| Content Type | Text |
| Resource Type | Article |
