Event Description

The stability of stars lying in a stellar sequence has been studied both with direct eigenvalue calculations as well as with an easier method involving the mass-radius curve. Both methods were thought to be equivalent, until a two-component equation of state was proposed which yielded "strange dwarf" stars which were deemed stable by the eigenvalue calculation, but not the mass-radius criterion. After a review of stellar structure, I will discuss the application of both stability analysis methods to these "strange dwarf" stars, and show that they are not stable to radial oscillations.