Abstract
Stellar pulsation in combination with radiation pressure on dust is proposed as the mechanism causing mass loss in Mira variables and an expression for the mass loss rate in terms of the basic stellar parameters mass and photospheric radius derived which leads to an acceleration of the mass loss rate in time as suggested by observations. Upper Asymptotic Giant Branch evolution with such a mass loss is presented. A model period distribution for classical Miras as well as a model 1612 MHz OH luminosity function for (OH/IR) Miras in the solar neighbourhood are fitted to observed ones. The time dependence of the past star formation rate and the average past star formation rate needed are in good agreement with those derived from totally different kinds of data.
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© 1986 D. Reidel Publishing Company
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Bedijn, P.J. (1986). From Miras to Planetary Nebulae: A Model of Mass Loss. In: Israel, F.P. (eds) Light on Dark Matter. Astrophysics and Space Science Library, vol 124. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-4672-9_27
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DOI: https://doi.org/10.1007/978-94-009-4672-9_27
Publisher Name: Springer, Dordrecht
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