Physics
Scientific paper
Jul 1971
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1971rspta.270..117g&link_type=abstract
Philosophical Transactions for the Royal Society of London. Series A, Mathematical and Physical Sciences, Volume 270, Issue 1202
Physics
Scientific paper
A number of time profiles are presented which show how the flux of radiation in the wavelength bands 0.1 to 0.3 nm, 0.3 to 0.9 nm, 0.8 to 1.6 nm and at 30.4 nm change during flares. The first sign of a flare is often a decrease of flux at 30.4 nm followed by an increase in the X-ray emission. In general, the higher the photon energy, the earlier the peak flux is reached, although any increase observed at 30.4 nm seems to peak before the X-ray flux. It is concluded that a model in which a mass of gas in the upper chromosphere is heated by shock waves or incident energetic particles does not explain the observations. What appears to be a more suitable model is suggested. Cool plasma from low in the chromosphere passes through a region of magnetic instability and is heated during the passage. In this way the material of the X-ray emitting region is heated to a high temperature a little at a time. The intensity of X-rays observed in each waveband is proportional to the volume of gas produced up to that time at the corresponding temperature. As the instability decays the gas passing through it can no longer be heated to the temperatures reached earlier and the emission of longer wavelength X-rays becomes dominant. The emission of γ -rays and radio waves can also be explained
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