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Evolution of H a Flare Kernels and Energy Release

Evolution of H a Flare Kernels and Energy Release. Ayumi ASAI Nobeyama Solar Radio Observatory, NAOJ 6 th Solar-B Science Meeting November 11, 2005 @Kyoto. What can we learn from Flare Kernels/Ribbons?. 2001-Apr-10 flare (Hida Obs.). Evolution of flare ribbons

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Evolution of H a Flare Kernels and Energy Release

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  1. Evolution of Ha Flare Kernels and Energy Release Ayumi ASAI Nobeyama Solar Radio Observatory, NAOJ 6th Solar-B Science Meeting November 11, 2005 @Kyoto

  2. What can we learn from Flare Kernels/Ribbons? 2001-Apr-10 flare (Hida Obs.) Evolution of flare ribbons  Information on Magnetic reconnection magnetic reconnection (Carmichael 1964; Sturrock 1966; Hirayama 1974; Kopp-Pneuman 1976)

  3. What can we learn from Flare Kernels/Ribbons? • Precipitation of accelerated particles into the chromosphere HXR emissions and Ha kernels Precipitation of nonthermal particles HXR Ha kernel corona Ha kernels  Information on particle acceleration chromoshere bremsstrahlung rapid thermalization What kind of information, and how, we can derive from the Ha observations on flare ribbons and kernels?

  4. 1. Conjugacy of Ha Footpoints Asai et al. 2003 • Nonthermal particles and thermal conduction bombard the chromospheric plasma at both the footpoints simultaneously The temporal evolutions of the footpoints are similar to each other • We identify the conjugated pairs of the footpoints which show similar light curves ? N S simultaneously brighten red:positive, blue:negative

  5. Focus on Each Pair Movement of the site of energy release t

  6. 2. Energy Release Rate Asai et al. 2004 Reconnection model indicates • estimate of the amount of the released energy, by using observable values to test the reconnection model • compare the derived energy release rate with HXR/microwave light curves Empirically, it is said that

  7. Energy Release Rate Electric Field Bc  conservation of magnetic flux Bp Poynting Flux Ha flare ribbons I estimate the energy release rate, by using observable values (Bp, vf)

  8. Reconnection Rate and Poynting Flux microwave HXR reconnection rate An HXR burst occurred on the slit (05:19 UT). Poynting flux B v B2 v

  9. Reconnection Rate and Poynting Flux microwave HXR reconnection rate An HXR burst occurred on the slit (05:26 UT). Poynting flux

  10. HXR/microwave Emission HXR sources flare ribbons Ha image Energy Release Rate

  11. Quantitative Estimation W2 E2 W2 E2 W1 Comparison of Poynting and Electric Field (Reconnection Rate) between the Ha kernels with HXR sources and those without ones E1 W3 E3 W4 E4

  12. 3. Ha Kernel Spectroscopy Ichimoto & Kurokawa 1984 Ha spectrum • Ha line is shifted red-ward red-asymmetry • velocity : 50-100 km/s flare X-ray corona Ha compression chromosphere Ha line l

  13. Red-Asymmetry Map • Ha +1.5A, -1.5A • we calculated as an indicator of r.a. • all over the flare ribbon, the tendency of r.a. is seen map

  14. Scatter Plot (intensity vs RA) intensity of Ha kernel blue red strong asymmetry @outer edges of the flare ribbon The downflow velocity is roughly about 30 km/s.

  15. Red Asymmetry l

  16. Summary • We can learn from Ha flare kernels/ribbons: • Site and timing of energy release by identifying conjugated footpoints • Energy release rate, by using the separation motions of two ribbons and the photospheric magnetic field strengths • Dynamics at the footpoints by the red-asymmetry distribution

  17. Thank you!

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