1. G. Nita 1 G. Fleishman 1, A. Kuznetsov 2, E. Kontar 3, D. Gary 1 1 New Jersey Institute of Technology, Physics, Newark- NJ, USA. 2 Institute of Solar-Terrestrial Physics, Irkutsk, Russia. 3 University of Glasgow, Astronomy, Glasgow, United Kingdom.

2. What’s new?  Version running on Windows, Unix and Mac platforms already available on SSW  Ability to import numerically defined chromospheric and coronal models  Integrated tools for generating data-driven chromospheric and coronal models (See my IUGG 4123 presentation on Friday for more details)  Generation of Microwave, EUV, and soft X-ray maps based on 3D models that may embed (still) analytical flaring loops models into numerical or analytical chromospheric and coronal models  A new upgrade of the SSW GX_Simulator package will be released on SSW before my GX Simulator lecture at the CESRA Summer School in Glasgow, August 24-28, 2015 What’s new?  Version running on Windows, Unix and Mac platforms already available on SSW  Ability to import numerically defined chromospheric and coronal models  Integrated tools for generating data-driven chromospheric and coronal models (See my IUGG 4123 presentation on Friday for more details)  Generation of Microwave, EUV, and soft X-ray maps based on 3D models that may embed (still) analytical flaring loops models into numerical or analytical chromospheric and coronal models  A new upgrade of the SSW GX_Simulator package will be released on SSW before my GX Simulator lecture at the CESRA Summer School in Glasgow, August 24-28, 2015

6. SOHO-MDI

7. OVSA 2.8GHz

8. OVSA 8.6GHz

9. RHESSI 12-25 MeV

11. X-ray 15keV model on RHESSI 12-25 keV OVSA image at 5.6 GHz on microwave 5.6 GHz model X-ray 15keV model on microwave 5.6GHz model RHESSI 12-25keV on OVSA 5.6 GHz

12.  3D modeling along with additional MW imaging and spectral data help to much better constrain the source model.  3D modeling confirms that the relatively displaced HXR and MW emissions are produced by co-spatial electron distributions.  MW-producing electron energy distribution is substantially harder than the HXR-producing ones.  In addition, by comparing rise and peak time models (not detailed here), we found that the fast electron spatial distribution width increases with time as the flare progresses.