1. Flare waves and the impulsive phase H. S. Hudson Space Sciences Laboratory University of California, Berkeley

2. Global Waves Interplanetary shock (SSC) * ; Type II burst; Moreton wave; seismic wave Major controversy on the interpretation of the metric type II and Moreton wave: is it a blast wave (two-wavism) or is it a CME-driven bow shock (one-wavism)? Wang-Zhang (2007) and Gopalswamy et al (2009) lists of CMEless X-class flares (cf. de La Beaujardière et al., 1994). * Storm Sudden Commencement

3. The “impulsive” phase Synchrotron radiation and hard X-ray bremsstrahlung Deep atmospheric effects (the UV/WL/IR emission) Non-thermal signatures The Neupert effect:

4. The “impulsive” phase CfA 1/13/10 Benz, 2002http://sprg.ssl.berkeley.edu/~tohban/browser

5. The Carrington Flare, 1859 CfA 1/13/10 (Chapman & Bartels)

6. CfA 1/13/10 (Chapman & Bartels)

7. Moreton Wave 6 Dec. 2006

9. 9 Subtracted Doppler Images (R-B Wing) Showing Down-Up Pattern 18:44 UT 18:47 UT 18:50 UT18:52 UT

10. 1844 UT The wave appears near the peak of the impulsive phase of the high-energy flare … Kaufmann et al. (2008)

11. Metric type II burst frequency time Slow drift to low frequencies Plasma frequency Shock acceleration of e -

12. Seismic Waves

13. Seismic Wave, 9 July 1996 (Kosovichev & Zharkova 1997)

14. Seismic Wave, 29 October 2003 (Donea & Lindsey 2005)

15. Seismic Wave, 15 January 2005 (Moradi et al. 2007)

16. Comparison of wave energies* IP shock: ~10% (Mewaldt) Moreton wave: >10 -4 (Gilbert) Seismic wave: ~10 -4 (Lindsey) *based on CME = flare = 1 (Emslie et al. 2005)

17. Magnetic changes during flares “Confusogram” legend: 10x10 2.5” pixels 240 minutes time base 500 G magnetic range (Sudol & Harvey 2005)

18. CfA 1/13/10 TRACE: dimming, implosion, oscillations

19. Wave tracing The Huyghens principle is necessary and sufficient (Wills-Davey & Thompson et al. 1999) Using it we can track either coronal or seismic waves back to the source The holographic technique works well for seismic waves

20. CfA 1/13/10 Flare/CME timing Zarro et al 1999Zhang et al 2001 DimmingCME speed vs time

21. CfA 1/13/10 Flare energy Woods et al 2004 Hudson et al 2006 In time In space

22. Cartoons CfA 1/13/10 Hudson 2000 Welsch 2008 Fletcher & Hudson 2008 Liu et al. 2007 http://solarmuri.ssl.berkeley.edu/~hhudson/cartoons

23. Wave origins The coronal wave could be either a blast wave (Uchida) or else a CME bow wave The origin of the coronal wave could be either in a pressure pulse, or via the Lorentz force - n.b. the corona has low plasma beta The seismic wave requires momentum transfer at or below the photosphere “…CMEs display an impulsive acceleration phase that coincides very well with the flare’s rise phase…” (J. Zhang et al., 2001)

24. CMEless X-class flare Gopalswamy et al. 2009

25. CMEless X-class flares Gopalswamy et al. 2009

26. LASCO shock signatures Ontiveros & Vourlidas. 2009

27. 1999 April 2 Examples from Vourlidas et al. 2003

28. Coronal waves CMEless flares have an upper cutoff in energy, implying environmental control of CME occurrence The CME acceleration phase matches the flare impulsive phase The lack of type II bursts with CMEless X-class flares implies that the Uchida-type wave is too weak

29. An interesting physics problem In Uchida theory, the coronal wave refracts into the chromosphere to produce the Moreton wave In the CME bow shock signature, this physics is different and needs to be worked out - The math may have been done by Kelvin, but it is not easy to identify in modern literature

30. Conclusions Coronal and seismic waves originate in the impulsive phase of a flare A CME (ie, unconstrained perpendicular outflow) is necessary for the generation of a coronal wave The waves in general illuminate the nature of the flare/CME restructuring There are some theoretical problems - behavior of shock flanks - conjecture on vector field change