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Soft X-ray observations of global waves Khan-Aurass 2002 Narukage et al. 2002 Hudson et al. 2002
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Solar shock: Type II burst
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Moreton-Ramsey wave and EIT wave Thompson et al., 2000
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X-ray observation of a global wave Wave propagation tells us about coronal structure The innermost (earliest) motions tell us about the flare process itself
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May 6, 1998 FOV 10 arc min
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SOHO/ EIT
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Uchida’s 1968 model
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S.W. Uchida A.R.
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What caused the blast wave? In principle we can see all of the process in soft X-rays The earliest manifestation of the May 6 wave is close (10 4 km) to the flare core But… it is significantly displaced from the core
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Implosion conjecture At low , the coronal energy is purely B 2 /8 During a flare, there’s no time for energy transport through the photosphere Therefore, some field lines must shorten
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Isomagnetobars Closed field lines Open field lines How low- implosions must work
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