Fig 3 - uploaded by John Butler
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The energy density (1015 erg a-1 IIz~l) versus wavelength at two times during the impulsive phase of the flare of 28 Feb 1985. Note that since the U, 13, V, R and I bands were not measured simultaneously, wc have interpolated fluxes to a common time through straight line fits to successive points. Superimposed is the energy spectrum for optical syn chrotron emission with a power-law energy distribution of 7 = 4.5 (-), free-free emission model with T -1.4 104 I\ (----) and the bound-free emission model with T = 1.4 104 K (..... ) for the data at 22:35:10 UT.
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Relative energies are given for the U,B,V,R and I bands for a 3.8 magnitude U-band flare observed on the dwarf dMe star Gl 234 AB on 28 Feb. 1985. This flare had a 45 second rise time and 20 minute decay time. The total flare energy from all five bands during the flare was 7×1031erg, 34% of this total was from the U-band and 20% from the two near i...
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Context 1
... the temperature to be 1.4 1 0 4Iif and the expression for optically thin free-free emission, we find that this model also fits the continuum slope for the observations at 22:35:10 UT. A slightly higher temperature of 3 1 0 4 K is required for the data taken at 22:35:30 UT. The energy distribution versus wavelength for both models is given on Fig. 3. In additional to the above mechanism, we consider bound-free emission, with again the best fit tc the data been given by Te = 1.4 104/ i . The above analysis however considers only the spectral distribution of the emission, below we discuss the energy content and number density implied by the above three ...
Context 2
... the temperature to be 1.4 1 0 4Iif and the expression for optically thin free-free emission, we find that this model also fits the continuum slope for the observations at 22:35:10 UT. A slightly higher temperature of 3 1 0 4 K is required for the data taken at 22:35:30 UT. The energy distribution versus wavelength for both models is given on Fig. 3. In additional to the above mechanism, we consider bound-free emission, with again the best fit tc the data been given by Te = 1.4 104/ i . The above analysis however considers only the spectral distribution of the emission, below we discuss the energy content and number density implied by the above three ...
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