Pulsational properties of post-AGB stars

Details Pulsational properties of post-AGB stars Pulsational properties of post-AGB stars

Oct 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aca....43..431z&link_type=abstract

Acta Astronomica, vol. 43, no. 4, p. 431-440

Astronomy and Astrophysics

Astronomy

10

Cepheid Variables, Hertzsprung-Russell Diagram, Hydrodynamics, Pulsars, Stellar Luminosity, Stellar Mass, Stellar Models, Supergiant Stars, Nonlinear Systems, Opacity, Stellar Temperature, Systems Stability

Scientific paper

Linear stability analysis and hydrodynamic calculations are performed for post-asymptotic giant branch star models using the new OPAL opacities of Iglesias et al. The linear pulsational calculations show that for low mass stars with L/M greater than 104 solar luminosity/solar mass the low order radial modes are unstable across the whole Hertzsprung-Russell diagram. Excited are radial fundamental mode and first overtone, and in the intermediate temperature range (log(Teff) approximately = 4.2) higher overtone modes become excited. With the new opacities the instability region is not confined to the extension of the Cepheid instability strip but extends much further towards higher effective temperatures. The behavior on nonlinear pulsations in selected models is presented. These calculations show that at higher temperatures the nonlinear models exhibit low amplitude approximately = 0.001 - 0.04 semiregular pulsations. The amplitudes are higher close to the regions where the driving in the H/He ionization or Z-bump zones is most efficient. In the intermediate temperature range the amplitudes are much smaller.

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