Dynamic Magnetography of Solar Flaring Loops

Details Dynamic Magnetography of Solar Flaring Loops Dynamic Magnetography of Solar Flaring Loops

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.1522f&link_type=abstract

American Astronomical Society, SPD meeting #40, #15.22; Bulletin of the American Astronomical Society, Vol. 41, p.839

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The coronal magnetic field is a key parameter controlling most solar flaring activity, particle acceleration and transport. However, unlike photospheric and chromospheric magnetography data, 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 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.
Anticipating a large breakthrough in the radio imaging spectroscopy observations, which will become possible soon due to the next generation of the radio instruments, we develop a practical forward fitting method based on the SIMPLEX algorithm with shaking that allows reliable derivation of the magnetic field and other parameters along a solar flaring loop using microwave imaging spectroscopy of gyrosynchrotron emission. We illustrate the method using a model loop (the subject of another presentation at this meeting, Nita et al., abstract # 09-A-57-SPD40) with spatially varying magnetic field, filled with uniform ambient density and an evenly distributed fast electron population with an isotropic, power-law energy distribution.
This work was supported in part by NSF grants AST-0607544 and ATM-0707319 and NASA grant NNG06GJ40G to New Jersey Institute of Technology

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