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EVE and RHESSI H. S. Hudson Space Sciences Laboratory, University of California, Berkeley, USA RHESSI, April 5, 2011
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Outline RHESSI, April 5, 2011 0) SOL2010-06-12T00:57 as seen by HMI 1)What is EVE? 2) How good is EVE? 3)What can we learn from EVE and RHESSI?
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SOL2010-06-12T00:57 (HMI) RHESSI, April 5, 2011 Martinez-Oliveros et al. 2011
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The ESP component of EVE RHESSI, April 5, 2011
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The ESP component of EVE RHESSI, April 5, 2011
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The ESP component of EVE RHESSI, April 5, 2011
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The ESP component of EVE RHESSI, April 5, 2011
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ESP fluxes for SOL2010-06-12 RHESSI, April 5, 2011
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The MEGS component of EVE RHESSI, April 5, 2011
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The MEGS component of EVE RHESSI, April 5, 2011
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EVE 304A for SOL2010-06-12 RHESSI, April 5, 2011 RHESSI 100 keV EVE 30.4 nm
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EVE 304A for SOL2010-06-12 RHESSI, April 5, 2011
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EVE 304 Doppler sensitivity RHESSI, April 5, 2011 1 pm = 1 km/s?
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EVE 304A for SOL2010-06-12 RHESSI, April 5, 2011
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EVE 304A for SOL2010-06-12 RHESSI, April 5, 2011
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He 304 Charge Exchange RHESSI, April 5, 2011 Peter et al. 1991
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SOL2010-06-12 Charge Exchange RHESSI, April 5, 2011
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SOL2010-06-12 Charge Exchange RHESSI, April 5, 2011
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SOL2011-02-15 Fe XXIV RHESSI, April 5, 2011
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SOL2011-02-15 Fe XXIV RHESSI, April 5, 2011
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What can we learn from EVE and RHESSI? UV/EUV energy distribution for WLF/HXR Charge-exchange observations of particles at.01-1 MeV/nucleon Transition-region explanation of 511 keV line width Flare dynamics, with big doses of imaging and modeling RHESSI, April 5, 2011
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Electrodynamic mapping of the solar interior to the corona RHESSI, April 5, 2011 Collisionality drops precipitously Hydrogen ionizes Plasma beta plummets Structurally important radiation escapes Vertical currents threading the photosphere carry the non-potential energy Recall debate between Parker and Melrose in ApJ (1996)
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