Non-adiabatic Spherical Pulsations
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When a star oscillates, its mass elements will generally not change their properties adiabatically. The outward-going heat flow, as well as the nuclear energy production, is modulated by the rhythm of the pulsation and both effects cause deviations from adiabaticity. However, since the pulsation takes place on the hydrostatic time-scale, which is short compared to τKH, the deviations from adiabaticity should be small in most parts of the stellar interior. In order to demonstrate the main effects of the non-adiabatic terms on the equation of motion, we discuss them at first for the simple piston model.
KeywordsMain Sequence Stellar Model Ionization Zone Adiabatic Case Instability Strip
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