Nonlinear Dynamics of Instabilities in Radiatively Driven Stellar Winds

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All stars lose mass from their surfaces by what has become known as stellar winds. In the case of cool stars, like the sun, the winds emanate from coronae, the tenuous outermost gaseous layers of those stars; and these winds are ultimately due to energy deposited from lower layers into the coronae. In the case of hot and luminous stars, the winds are driven by photons that are absorbed by gas particles constituting the stars' atmospheres. This absorption of photons can lead to dynamic instabilities and emission of radiation from radio to X-ray frequencies, offering opportunities for indirectly observing the wind generating mechanism. The Principal Investigator proposes to model this mechanism numerically and analytically.