A&A 635, A173 (2020) Astronomy https://doi.org/10.1051/0004-6361/201937150 & © ESO 2020 Astrophysics Stellar wind models of central stars of planetary nebulae J. Krtickaˇ 1, J. Kubát2, and I. Krtickovᡠ1 1 Ústav teoretické fyziky a astrofyziky, Masarykova univerzita, Kotlárskᡠ2, 611, 37 Brno, Czech Republic e-mail:
[email protected] 2 Astronomický ústav, Akademie vedˇ Ceskéˇ republiky, Fricovaˇ 298, 251 65 Ondrejov,ˇ Czech Republic Received 20 November 2019 / Accepted 26 February 2020 ABSTRACT Context. Fast line-driven stellar winds play an important role in the evolution of planetary nebulae, even though they are relatively weak. Aims. We provide global (unified) hot star wind models of central stars of planetary nebulae. The models predict wind structure including the mass-loss rates, terminal velocities, and emergent fluxes from basic stellar parameters. Methods. We applied our wind code for parameters corresponding to evolutionary stages between the asymptotic giant branch and white dwarf phases for a star with a final mass of 0:569 M . We study the influence of metallicity and wind inhomogeneities (clumping) on the wind properties. Results. Line-driven winds appear very early after the star leaves the asymptotic giant branch (at the latest for T 10 kK) and eff ≈ fade away at the white dwarf cooling track (below Teff = 105 kK). Their mass-loss rate mostly scales with the stellar luminosity and, consequently, the mass-loss rate only varies slightly during the transition from the red to the blue part of the Hertzsprung–Russell diagram. There are the following two exceptions to the monotonic behavior: a bistability jump at around 20 kK, where the mass- loss rate decreases by a factor of a few (during evolution) due to a change in iron ionization, and an additional maximum at about 1 1 Teff = 40 50 kK.