Advances in Plasma Astrophysics, Giardini-Naxos, 6-10 Sept. 2010 3D Modeling of Solar Flaring Loops New Interactive Solar Flare Modeling and Advanced Radio

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 ToolsGregory D. Fleishman,

Gelu M. Nita, & Dale E. GaryNJIT



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.



Modeling. Flares.



Fitted byEquation of the radiation transfer is solved numerically for each line of sight: Fast GS Codes, see poster by A.KUZNETSOV









Fit to Model Comparison





OVSA UpgradeTable 1: OVSA Upgrade Specifications

Frequency range 1 – 18 GHz

Number of data channels

2 (dual polarization)

IF bandwidth 500 MHz per channel

Frequency resolution Raw: 122 kHz (4096 spectral channels)

Science: ~50 MHz

Time resolution Sample time: 20 msFull Sweep: 680 ms

Polarization Full Stokes (IQUV)

Number correlator inputs per data channel

16

Number and type of antennas

Five 2-m equatorialEight 2-m azelTwo 27-m equatorial

(night-time and cal. only)

Angular resolution 36/GHz × 56/GHz arcsec

Array size 1.5 km EW x 1.1 km NS



Image Improvement

c)a) b)



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.

Documents

Advances in Plasma Astrophysics, Giardini-Naxos, 6-10 Sept. 2010 3D Modeling of Solar Flaring Loops New Interactive Solar Flare Modeling and Advanced Radio