Stellar wind models of central stars of planetary nebulae

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F20%3A00114456" target="_blank" >RIV/00216224:14310/20:00114456 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.1051/0004-6361/201937150" target="_blank" >https://doi.org/10.1051/0004-6361/201937150</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201937150" target="_blank" >10.1051/0004-6361/201937150</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Stellar wind models of central stars of planetary nebulae

Popis výsledku v původním jazyce

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.

Název v anglickém jazyce

Stellar wind models of central stars of planetary nebulae

Popis výsledku anglicky

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.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

Výsledek vznikl pri realizaci vícero projektů. Více informací v záložce Projekty.

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2020

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astronomy & Astrophysics

ISSN

0004-6361

e-ISSN

—

Svazek periodika

635

Číslo periodika v rámci svazku

APR 2 2020

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

14

Strana od-do

1-14

Kód UT WoS článku

000526658700001

EID výsledku v databázi Scopus

2-s2.0-85083308923