• 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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Back Projection

Clean

Pixon

Forward Fit

MEM NJIT

VIS-Forward Fit

UV smooth

Electron Map

1. Fast2. Easy to calculate uncertainties3. Lease details than other methods4. Explain results carefully

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.

RHESSI visibilities are very good at getting 1st 3 moments of simple sources

Flux, size, location

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

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

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

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