1. Advances in Plasma Astrophysics, Giardini-Naxos, 6-10 Sept. 2010 3D Modeling of Solar Flaring Loops New Interactive Solar Flare Modeling and Advanced Radio Inversion Tools Gregory D. Fleishman, Gelu M. Nita, & Dale E. Gary NJIT

2. Advances in Plasma Astrophysics, Giardini-Naxos, 6-10 Sept. 2010 3D Modeling of Solar Flaring Loops Motivation The coronal magnetic field is a key parameter controlling most solar flaring activity, particle acceleration and transport. However, although photospheric and some chromospheric magnetography data are available, there is currently a clear lack of quantitative information on the coronal magnetic field in the dynamically flaring region, which complicates the detailed modeling of fundamental physical processes occurring in the corona. It has been understood, and often proposed, that the coronal magnetic field along with fast electron distribution can in principle be evaluated from the microwave gyrosynchrotron radiation, which is indeed sensitive to the instantaneous magnetic field strength and orientation relative to the line of sight and to the fast electron spectrum. To fully explore the data flows expected from new radio instruments it is urgently necessary to bring the theory and the modeling up to date with the new demands of anticipated observations.

3. Advances in Plasma Astrophysics, Giardini-Naxos, 6-10 Sept. 2010 3D Modeling of Solar Flaring Loops Modeling. Flares.

4. Advances in Plasma Astrophysics, Giardini-Naxos, 6-10 Sept. 2010 3D Modeling of Solar Flaring Loops Fitted by Equation of the radiation transfer is solved numerically for each line of sight: Fast GS Codes, see poster by A.KUZNETSOV

5. Advances in Plasma Astrophysics, Giardini-Naxos, 6-10 Sept. 2010 3D Modeling of Solar Flaring Loops

6. Advances in Plasma Astrophysics, Giardini-Naxos, 6-10 Sept. 2010 3D Modeling of Solar Flaring Loops

7. Advances in Plasma Astrophysics, Giardini-Naxos, 6-10 Sept. 2010 3D Modeling of Solar Flaring Loops

8. Advances in Plasma Astrophysics, Giardini-Naxos, 6-10 Sept. 2010 3D Modeling of Solar Flaring Loops Fit to Model Comparison

9. Advances in Plasma Astrophysics, Giardini-Naxos, 6-10 Sept. 2010 3D Modeling of Solar Flaring Loops

10. Advances in Plasma Astrophysics, Giardini-Naxos, 6-10 Sept. 2010 3D Modeling of Solar Flaring Loops OVSA Upgrade Table 1: OVSA Upgrade Specifications Frequency range1 – 18 GHz Number of data channels 2 (dual polarization) IF bandwidth500 MHz per channel Frequency resolutionRaw: 122 kHz (4096 spectral channels) Science: ~50 MHz Time resolutionSample time: 20 ms Full Sweep: 680 ms PolarizationFull Stokes (IQUV) Number correlator inputs per data channel 16 Number and type of antennas Five 2-m equatorial Eight 2-m azel Two 27-m equatorial (night-time and cal. only) Angular resolution 36/ GHz × 56/ GHz arcsec Array size1.5 km EW x 1.1 km NS

11. Advances in Plasma Astrophysics, Giardini-Naxos, 6-10 Sept. 2010 3D Modeling of Solar Flaring Loops Image Improvement c) a) b)

12. Advances in Plasma Astrophysics, Giardini-Naxos, 6-10 Sept. 2010 3D Modeling of Solar Flaring Loops Conclusions Using newly developed 3D direct modeling and forward fitting inversion tools, for the first time we demonstrated that the magnetic field data can reliably be recovered from the imaging spectroscopy data on the GS emission of solar flares, even though a number of important issues have yet to be analyzed to convert this method to a routine, practical tool. Building the new radio instruments is crucially important for solving the key problems in the solar physics. Anticipated developments in solar radio astronomy will bring the solar community to the Dynamic Imaging Spectroscopy era.