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

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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

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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

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