1. Evidence of Chromospheric Evaporation in a Neupert-type Flare NING Zongjun ningzongjun@pmo.ac.cn Purple Mountain Observatory, China

2. Flare Model corona chromosphere HXR Evaporation SXR Neupert Effect It is necessary to see the evidence of chromospheric evaporation in a Neupert-type event. Based on this concept, we try: 1.To prove that the flare does follow the Neupert effect; 2.To look for the evidence of evaporation. Hot

3. The event we select 2004. Oct. 30 M3.3 03:23 — 03:37 UT (GOES) N14W15 (disk event) 10691

4. 2004 Oct.30 solar flare RHESSI_HXR GOES_SXR Temperature EM Low cutoff Electron spectral index Thermal E Nonthermal E

5. 1. How to test the Neupert effect from these parameters?

6. Methods to test the Neupert effect 1.Comparison: the maximum of the SXR derivative with the HXR maximum (e.g. Dennis et al. 1985) 2.Comparison: time difference between the SXR maximum and the HXR end (e.g. Veronig et al. 2002) 3.Correlation: I. Between the SXR derivative and HXR light curve (e.g. Ning et al. 2009) II. Between the thermal energy derivative and HXR light curve (e.g. Ning et al. 2008) III. Between thermal energy derivative and nonthermal energy profiles (e.g. Ning 2009, submitted)

7. Correlation HXR SXR derivative Thermal E derivative Nonthermal energy 0.71 0.74 This event does follow the Neupert effect!

8. 2. Then we look for the evidence of chromospheric evaporation in this flare.

9. Evidence of evaporation 1.Seen on radio dynamics high frequency cutoff and positively drifting (e.g. Aschwanden & Benz 1995) II. HXR footpoints move close and finally merge together (disk event, e.g. Ning et al. 2009) 2.Seen by EUV and Ha I. EUV red-shift on the edge of ribbons (e.g. Czaykowska et al. 1999) II. broad Ha width on the edge of ribbons(e.g. Li & Ding 2004) 3.Seen by HXR I. HXR footpoint sources tend to rise up and finally merge together (limb event, e.g. Liu et al. 2006)

10. Evidence of evaporation 1.Seen on radio dynamics high frequency cutoff and positively drifting 2.Seen by EUV and Ha I. EUV red-shift on the edge of ribbons II. broad Ha width on the edge of ribbons 3. Seen by HXR I. HXR footpoint sources tend to rise up and finally merge together (limb event, e.g. Liu et al. 2006)

11. Evidence of evaporation 1.Seen on radio dynamics high frequency cutoff and positively drifting 2.Seen by EUV and Ha I. EUV red-shift on the edge of ribbons II. broad Ha width on the edge of ribbons 3.Seen by HXR I. HXR footpoint sources tend to rise up and finally merge together (limb event, e.g. Liu etal. 2006) II. HXR footpoints move close and finally merge together (disk event, e.g. Ning et al. 2009) 2004 Oct. 30

12. Projection correction Assumption: semi-circular loop Evaporation speed: (S)632 km/s & (N)397 km/s

13. Summary 2004. Oct. 30 solar flare: 1.This event shows the Neupert effect. 2.This event exhibits the double footpoints movement close together and finally mergence into a single source at the same position of the loop-top source, which is thought to be the evidence of the chromospheric evaporation at HXR. (Ning et al. 2009 submitted)

14. Thanks!