H2.

A large solar are can be roughly modeled as emission from an optically-thin thermal plasma in collisional ionization equilibrium from a cylindrical region some 5 at 1C\"1 km in diameter by about 5 K 10'1 km high and at a temperature of ll]? K. For simplicity, one can assume the emission from this plasma as being dominated by the bremstrahlung {ff] emission. The radiation energy Hm: from such a region is about 0.1 erg cm'2 s1 at the Earth integrated over all energies. Please answer the following questions: 1rhe's-"hat are the total ff emissivity1 electron density. energy density, and cooling timescale for the plasma? If the magnetic eld in the aring region is 2 X 103 gauss, how does the magnetic energy density compare to the energy density in the plasma?I