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Multi-Wavelength Studies of Flare Activities with Solar-B ASAI Ayumi Kwasan Observatory, Kyoto University Solar-B Science February 4, 2003.

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Presentation on theme: "Multi-Wavelength Studies of Flare Activities with Solar-B ASAI Ayumi Kwasan Observatory, Kyoto University Solar-B Science February 4, 2003."— Presentation transcript:

1 Multi-Wavelength Studies of Flare Activities with Solar-B ASAI Ayumi Kwasan Observatory, Kyoto University Solar-B Science February 4, 2003

2 Magnetic Reconnection Model Magnetic Reconnection elemental process for solar flares To solve the mechanism, quantitative studies are needed.  Solar-B’s target

3 Today’s Topic Using various phenomena, we derive the information about the energy release via reconnection. I present the estimation of the energy release rate at flares, by multi-wavelength studies of flares. Analyzed flares 2000-April-10 Flare (X2.3) 2002-July-23 Flare (X4.8) 2000-November-24 Flare (X2.3)  Suggestion for the observations with Solar-B

4 Energy Release Rate Time profiles of HXR and microwave intensities are well fitted with that of dE/dt Reconnection model indicates B c : coronal magnetic field strength v in : inflow velocity A : area of the reconnection region I estimate the energy release rate, and compare it with nonthermal light curves.

5 Data Observational Data H  ・・ Kwasan Observatory, Sartorius Telescope EUV ・・ TRACE (171, 195 Å image) magnetogram ・・ SOHO / MDI hard-X ray ・・ Yohkoh / HXT RHESSI HXRS (Czech) microwave ・・ Nobeyama Radioheliograph Sartorius Telescope

6 2001-April-10 Flare H  images taken with Sartorius Telescope East West Flare I ・ April 10, :10 UT ・ GOES X2.3 class NOAA 9415

7 Features of the Flare Microwave and HXR light curves show some bursts. The spatial distributions of H  kernels are different from those of HXR sources. H  image HXR sources HXT GOES NoRH Sartorius

8 Evolution of Flare Ribbons Neutral Line B v I estimate the reconnection rate v×B, and the Poynting flux v×B 2 as the representations of the energy release rates.

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

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

11 Summary I I have estimated the energy release rate from the separation motions of H  two ribbons and the photospheric magnetic field strengths. The estimated reconnection rate and the Poynting flux along each slit show good correlation with nonthermal burst.

12 2002-July-23 Flare Flare II ・ July 23, :15 UT ・ GOES X4.8 class ・ NOAA 0039 EUV(195 Å ) images taken with TRACE East West

13 Down Flow The timings of the down flows correspond to microwave/HXR bursts. Time slice image TRACE 195A microwave (NoRH 17GHz)

14 2000-November-24 Flare Time slice image This flare shows many plasmoid ejections, and each of them is ejected at the time corresponding to the HXR burst. Takasaki (2003) Yohkoh/SXT

15 Summary II Down flow motions and plasmoid ejections show some correlations with HXR/microwave bursts.  Strongly depend on the reconnection process.  More quantitative studies are still needed.

16 Observation with Solar-B SOT … XRT … EIS … collaboration with other satellite and ground based instruments Hida Obs., Nobeyama, RHESSI… H  images with high spatial resolution Magnetograms with high spatial resolution Observation of reconnection outflow, and density and temperature of the plasma Velocity field of the reconnection outflow


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