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It is possible that reconnection can occur multiple times along CS

It is possible that reconnection can occur multiple times along CS Plasmoids form as magnetic ‘islands’ between X-points Due to density and magnetic field strength decreasing with height, the majority of plasmoids are observed to rise. ?. ?. Back Projection Clean Pixon Forward Fit

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It is possible that reconnection can occur multiple times along CS

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  1. It is possible that reconnection can occur multiple times along CS • Plasmoids form as magnetic ‘islands’ between X-points • Due to density and magnetic field strength decreasing with height, the majority of plasmoids are observed to rise

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  4. Back Projection Clean Pixon Forward Fit MEM NJIT VIS-Forward Fit UV smooth Electron Map • Fast • Easy to calculate uncertainties • Lease details than other methods • Explain results carefully

  5. RHESSI visibilities are very good at getting 1st 3 moments of simple sources Flux, size, location First 3 moments are not always the full story. RHESSI cannot image complex sources, but visibilities may tell you that a few details are missing.

  6. Planning a New Mission Solar Vision 2020 A theorist's assessment/wish list of the future observational needs (Gordon Emslie) Key Interests: (a) thermal vs. nonthermal (b) acceleration (c) ion energy

  7. Problem Solved: (1) true shape of HXR spectra (2) Microflares do NOT heat the corona (3) Flare connects to CME Problem Advanced but need to dig more: (1) Thermal/Nonthermal transition in the electron distribution fucntion (2) HXR structure at very small spatial scales (3) Directivity/location of HXR sources (4) Physical parameters of acceleration region (n, T, B) (5) Electron maps, but not at stage to study variation of F(E, r, t) (6) (EM, T) analysis (7) Partion of flare energy, SEP shock-acceleration efficiency (8) Fourier-based Imaging Problem Uncovered: (1) nonthermal source in the corona (2) HXR/gamma-ray emission location different (3) gamma-ray redshift (4) Different electron spectra for radio and HXR

  8. Some thoughts of the new RHESSI: 0.1'' at 6.7 keV Focusing X-rays (lens of Si) Multiple Satellites 32 x 32 pix HXR imaging system (Bandler) 1k x 1k HXR Camera (<50 keV) @Brookhaven National Lab

  9. Current Status of RHESSI 3. Bob Lin: 2010 Mar 16, 07:27UT. Clock stopped Observation resumed on May 1, 2010 pure non-thermal loop-top source, acceleration region RHESSI now modeled up to 150 Kev RHESSI vs Hinode (Kruck, HXR kernels over G-band) Future, RHESSI will be there for the coming solar maximum the next generation will be launched around 2022. 4. We are able to image better than before 5. GH: Regression provision in Clean to improve normalization RHESSI data base at ETHZ moved to FHNW Cloud Solar Software (Nugget #131) HESPE, High Energy Solar Physics Dara in Europe grid 1 data, <4s time resolution

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