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@article{1692976,
author = {Krtička, Jiří and Kubát, Jiří and Krtičková, Iva},
article_location = {Les Ulis},
article_number = {APR 2 2020},
doi = {http://dx.doi.org/10.1051/0004-6361/201937150},
keywords = {stars: winds; outflows; stars: mass-loss; stars: early-type; stars: AGB and post-AGB; white dwarfs; planetary nebulae: general},
language = {eng},
issn = {0004-6361},
journal = {Astronomy & Astrophysics},
title = {Stellar wind models of central stars of planetary nebulae},
url = {https://doi.org/10.1051/0004-6361/201937150},
volume = {635},
year = {2020}
}
TY - JOUR
ID - 1692976
AU - Krtička, Jiří - Kubát, Jiří - Krtičková, Iva
PY - 2020
TI - Stellar wind models of central stars of planetary nebulae
JF - Astronomy & Astrophysics
VL - 635
IS - APR 2 2020
SP - 1-14
EP - 1-14
PB - EDP Sciences
SN - 00046361
KW - stars: winds
KW - outflows
KW - stars: mass-loss
KW - stars: early-type
KW - stars: AGB and post-AGB
KW - white dwarfs
KW - planetary nebulae: general
UR - https://doi.org/10.1051/0004-6361/201937150
L2 - https://doi.org/10.1051/0004-6361/201937150
N2 - 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-circle dot. 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-eff approximate to 10 kK) and fade away at the white dwarf cooling track (below T-eff = 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 T-eff = 40-50 kK. On the other hand, the terminal velocity increases from about a few hundreds of km s(-1) to a few thousands of km s(-1) during the transition as a result of stellar radius decrease. The wind terminal velocity also significantly increases at the bistability jump. Derived wind parameters reasonably agree with observations. The effect of clumping is stronger at the hot side of the bistability jump than at the cool side.Conclusions. Derived fits to wind parameters can be used in evolutionary models and in studies of planetary nebula formation. A predicted bistability jump in mass-loss rates can cause the appearance of an additional shell of planetary nebula.
ER -
KRTIČKA, Jiří, Jiří KUBÁT a Iva KRTIČKOVÁ. Stellar wind models of central stars of planetary nebulae. \textit{Astronomy \&{} Astrophysics}. Les Ulis: EDP Sciences, 2020, roč.~635, APR 2 2020, s.~1-14. ISSN~0004-6361. Dostupné z: https://dx.doi.org/10.1051/0004-6361/201937150.
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