{ "id": "1907.01230", "version": "v1", "published": "2019-07-02T08:32:42.000Z", "updated": "2019-07-02T08:32:42.000Z", "title": "Evolution and pulsations of population I post-AGB stars", "authors": [ "Yu. A. Fadeyev" ], "comment": "14 pages, 4 figures, accepted to Astron. Lett", "categories": [ "astro-ph.SR" ], "abstract": "Evolutionary calculations of population I stars with initial masses $M_0=1M_\\odot$, $1.5M_\\odot$ and $2M_\\odot$ were carried out up to the stage of the proto--planetary nebula. Selected models of post--AGB evolutionary sequences with effective temperatures $3.6\\times 10^3\\,\\mathrm{K}\\lesssim T_\\mathrm{eff}\\lesssim 2\\times 10^4\\,\\mathrm{K}$ were used as initial conditions in calculations of self--escited stellar oscillations. For the first time the sequences of hydrodynamic models of radially pulsating post--AGB stars were computed using the self--consistent solution of the equations of radiation hydrodynamics and time--dependent convection. Within this range of effective temperatures the post--AGB stars are the fundamental mode pulsators with period decreasing as the star evolves from $\\Pi\\approx 300$ day to several days. Period fluctuations are due to nonlinear effects and are most prominent at effective temperatures $T_\\mathrm{eff} < 5000$K. The amplitude of bolometric light variations is $\\Delta M_\\mathrm{bol}\\approx 1$ at $T_\\mathrm{eff} \\lesssim 6000$K and rapidly decreases with increasing $T_\\mathrm{eff}$. The theoretical dependence of the pulsation period as a function of effective temperature obtained in the study can be used as a criterion for the evolutionary status of pulsating variables suspected to be post--AGB stars.", "revisions": [ { "version": "v1", "updated": "2019-07-02T08:32:42.000Z" } ], "analyses": { "keywords": [ "effective temperature", "population", "bolometric light variations", "post-agb evolutionary sequences", "fundamental mode pulsators" ], "note": { "typesetting": "TeX", "pages": 14, "language": "en", "license": "arXiv", "status": "editable" } } }