Ongoing Issues

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(Spectral issues)
(Type III emission)
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==Type III emission==
==Type III emission==
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*threshold of electron density for Type III burst generation (Kontar)
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*threshold of electron density for Type III burst generation? (Kontar)
*Type III emission delay with respect to SEPs (up to 10 mins): ~1/3 of events are delayed, 1/3 on time, ~1/3 hard to say (Krucker).
*Type III emission delay with respect to SEPs (up to 10 mins): ~1/3 of events are delayed, 1/3 on time, ~1/3 hard to say (Krucker).
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==Gamma-rays==
==Gamma-rays==
*pair production in 1 MK plasma for 10 mins. How can plasma be so hot so low for such a long time? (Share)
*pair production in 1 MK plasma for 10 mins. How can plasma be so hot so low for such a long time? (Share)

Revision as of 23:33, 13 May 2009

Contents

Number problem


Pre-flare


Spectral issues


Type III emission


Gamma-rays


HXR footpoint issues

1. Timing: RHESSI should be able to do footpoint timing at the 0.1s level with visibilities (Hurford)

2. Flux ratios, spectral index differences: Double footpoint flares: do we have correlation between spectral index difference and flux ratios? --> Actually, some. Saint-Hilaire et al. (2008) have demonstrated that differences in column densities between leg of loops cannot explain all observed footpoint spectral index differences and flux ratios. Some other important mechanism is at play, most probably magnetic mirroring. Liu et al. (2008) basically agree, saying that neither a difference in column densities nor magnetic mirroring alone can explain all observations: we have interplay between the two (or there is even something else that comes into play).

3. Are spectral breaks the same for both footpoints?


Flare T, EM

Hottest temperatures in flares (45 MK) occur early in flare, at end of HXR emission (Neupert effect). EM goes on to rise and peaks much later (Caspi). In an event analysed by Saint-Hilaire et al. (2009), EM increases during more than 10 hours.


Neutral SEPs


Energetics


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