Linear and nonlinear models of Mira variable stars

Details Linear and nonlinear models of Mira variable stars Linear and nonlinear models of Mira variable stars

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982phdt.........3o&link_type=abstract

Ph.D. Thesis Iowa State Univ. of Science and Technology, Ames.

Astronomy and Astrophysics

Astrophysics

3

Astrophysics, Mira Variables, Stellar Models, Variable Stars, Hertzsprung-Russell Diagram, Pulses, Stellar Mass, Stellar Rotation, Turbulence

Scientific paper

A survey of linear, nonadiabatic models in the Mira instability region of the H-R diagram was carried out for solar masses ranging from 0.8 to 2.0, with effective temperatures from 2700 K to 3400 K and solar luminosities from 1500 to 7000. From this study period-mass-radius relations were derived for fundamental mode and first overtone pulsation; these relations can then be compared to observations. All models include molecular opacities and an opacity averaging scheme within each zone of rising and falling convective elements. In some models turbulent pressure was also included. The nonlinear behavior of several selected models was also investigated. A time-dependent modulation of the convective velocities was included in all cases. For the 0.8 solar mass model without turbulent pressure, pulsation reached a limiting amplitude but was distinctly aperiodic. When turbulent pressure was included in the 0.8 solar models, pulsation amplitudes increased without limit. For the 1.4 solar mass models studied, turbulent pressure was included and steady fundamental mode pulsation was obtained, but with amplitudes much smaller than are observed for Miras.

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