Nonlinear Dynamics of Instabilities in Radiatively Driven Stellar Winds

所有的恒星都会因为所谓的恒星风而失去表面的质量。对于温度较低的恒星，比如太阳，风是从这些恒星最外层脆弱的气体层日冕中发出的；这些风最终是由于能量从较低层沉积到日冕中。在炽热明亮的恒星中，风是由光子驱动的，光子被构成恒星大气层的气体粒子吸收。这种光子的吸收会导致动态不稳定和从无线电到x射线频率的辐射发射，为间接观察风的产生机制提供了机会。首席研究员建议对这一机制进行数值模拟和分析。

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.