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Uses of solar hard X-rays Basics of observations Hard X-rays at flare onset The event of April 18, 2001 Conclusions Yohkoh 10th Jan. 21, 2002Hugh Hudson,

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Presentation on theme: "Uses of solar hard X-rays Basics of observations Hard X-rays at flare onset The event of April 18, 2001 Conclusions Yohkoh 10th Jan. 21, 2002Hugh Hudson,"— Presentation transcript:

1 Uses of solar hard X-rays Basics of observations Hard X-rays at flare onset The event of April 18, 2001 Conclusions Yohkoh 10th Jan. 21, 2002Hugh Hudson, SPRC/UCB

2 Hard X-ray basics Hard X-rays come from bremsstrahlung Bremsstrahlung is inefficient, and electrons >20 keV dominate flare energetics Flare hard X-rays normally follow the Neupert effect Footpoints (often double) are prominent

3 Basics II Spectra look like power laws (may be broken) Impulsive-phase hard X-rays follow the Soft-hard-soft pattern Protons > 10 MeV now appear to resemble electrons > 20 keV energetically Also see “superhot” hard X-rays

4 Hot “Superhot” Broken power law Gamma rays “Broken up” Pi decay ? 1 keV 1 MeV1 GeV E f(E)

5 Another Neupert plot

6 A non-Neupert event

7 Conclusion Energy release in the impulsive phase coincides temporally with a distorted electron distribution function.

8 Neupert Effect - II Correlation plot for hard X-ray and soft X- ray peak fluxes, done for "slow LDEs"

9 A typical slow LDE, the “candle flame” flare (21-Feb-92)

10 Feb. 21 has a long “impulsive” phase - the Neupert effect

11 Conclusion The “impulsive phase” non-thermal effects occur in flares of all sizes and time scales.

12 Conclusion Soft-hard-soft spectral evolution is something fundamental that is modelable, but which has not yet been modeled.

13 September 24, 2001 HXT observed a rapidly-variable source with a soft spectrum at the onset phase

14 Conclusion There are strong suggestions that the basic physics of pre-flare excitation is not “heating,” but rather particle acceleration

15 April 18, 2001

16 Summary of uses I Footpoint connectivity Impulsive-phase energetics Coronal trapping Filament activation “Firm” X-rays

17 Summary of uses II Type I Type II Type III Type IV

18 Hot “Superhot” Broken power law Gamma rays “Broken up” Pi decay ? 1 keV 1 MeV1 GeV E f(E)

19 Reflecting hard X-ray telescope Zero background Infinite dynamic range Photometry limited by counting statistics Good spectral domain (to tens of keV) All technologies seem to be available


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