AAS 204th Meeting, June 2004
Session 71 Large-Scale Features of the Solar Corona
SPD Poster, Thursday, June 3, 2004, 9:20am-4:00pm, Ballroom

[Previous] | [Session 71] | [Next]

[71.04] Simulations of the Quiet Sun Emission at Metric and Decimetric Radio Wavelengths

C. Marqué (USRA-NRL), Y.M. Wang (NRL), A.F. Thernisien (USRA-NRL), A. Vourlidas, R.A. Howard (NRL)

In the metric and decimetric radio range, solar emission is dominated by non-thermal radiation from electron populations accelerated during flares or continuous processes. When the solar activity is low, mainly during the solar cycle minimum, the thermal emission from the corona can be mapped, and structures such as coronal holes, active regions or filament cavities can be observed. The radio thermal emission is sensitive to the electron density and temperature, and radio rays suffer refraction effects when their frequency is close to the local plasma frequency. A model of the electron density and temperature distribution is thus needed to compute the thermal radiation at a given frequency. Axisymetric and homogeneous electron density models have been successfully used for the last fourty years to described the basic properties of this thermal emission. Nevertheless, these density models are not suitable for describing the corona at a given date.

We present in this poster more realistic simulations using a Potential Field Source Surface extrapolation and realistic electron density distributions. Assuming hydrostatic equilibrium, the density is determined by the strength of the magnetic field and the length of the magnetic loops: n=n0(B,L)*f(r). Different n0 and f functions are used and the corresponding results are compared to real data.

[Previous] | [Session 71] | [Next]

Bulletin of the American Astronomical Society, 36 #2
© YEAR. The American Astronomical Soceity.