Multiple energetic injections in a strong spike-like solar burst |
| |
| Authors: | P Kaufmann E Correia J E R Costa B R Dennis G J Hurford J C Brown |
| |
| Institution: | (1) INPE: Instituto de Pesquisas Espaciais, CNPq, 12200 São José dos Campos, SP, Brazil;(2) Laboratory of Astronomy and Solar Physics, Solar Activity Branch, NASA-Goddard Space Flight Center, 20771 Greenbelt, MD, U.S.A.;(3) California Institute of Technology, 91125 Pasadena, CA, U.S.A.;(4) Department of Astronomy, The University, G12 8QQ Glasgow, UK |
| |
| Abstract: | An intense and fast spike-like solar burst was observed with high sensitivity in microwaves and hard X-rays, on December 18,1980, at 19h21m20s UT. It is shown that the burst was built up of short time scale structures superimposed on an underlying gradual emission, the time evolution of which showed remarkable proportionality between hard X-ray and microwave fluxes. The finer time structures were best defined at mm-microwaves. At the peak of the event the finer structures repeat every 30–60 ms (displaying an equivalent repetition rate of 16–20 s-1). The more slowly varying component with a time scale of about 1 s was identified in microwaves and hard X-rays throughout the burst duration. Similarly to what has been found for mm-microwave burst emission, we suggest that X-ray fluxes might also be proportional to the repetition rate of basic units of energy injection (quasi-quantized). We estimate that one such injection produces a pulse of hard X-ray photons with about 4 × 1021 erg, for   25 keV. We use this figure to estimate the relevant parameters of one primary energy release site both in the case where hard X-rays are produced primarily by thick-target bremsstrahlung, and when they are purely thermal, and also discuss the relation of this figure to global energy considerations. We find, in particular, that a thick-target interpretation only becomes possible if individual pulses have durations larger than 0.2 s. |
| |
| Keywords: | |
| 本文献已被 SpringerLink 等数据库收录！ |
|
