Abstract
The interior structure, the evolution, and the p-mode oscillation spectra of stellar models between 2.0 and 5 M☉ are presented. Interior details, including convective core and envelope growth and decay, the development of composition gradients, and the onset of hydrogen shell burning are shown to be testable by future asteroseismology observations. The stellar age and mass dependence of the large- and small-spacing oscillation frequencies are discussed. The dependencies of the structure and the oscillation spectra on composition and mixing length are also discussed. A new oscillation diagnostic for stellar mass is introduced.
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