New line-driven wind mass-loss rates for OB stars with metallicities down to 0.01 Z⊙

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F25%3A00639899" target="_blank" >RIV/67985815:_____/25:00639899 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/00216224:14310/25:00143042

Výsledek na webu

<a href="https://hdl.handle.net/11104/0370392" target="_blank" >https://hdl.handle.net/11104/0370392</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202556234" target="_blank" >10.1051/0004-6361/202556234</a>

Jazyk výsledku

angličtina

Název v původním jazyce

New line-driven wind mass-loss rates for OB stars with metallicities down to 0.01 Z⊙

Popis výsledku v původním jazyce

We provide new line-driven wind models for OB stars with metallicities down to 0.01 Z(circle dot). The models were calculated with our global wind code METUJE, which solves the hydrodynamical equations from nearly hydrostatic photosphere to supersonically expanding stellar wind together with the equations of statistical equilibrium and the radiative transfer equation. The models predict the basic wind parameters, namely, the wind mass-loss rates and terminal velocities just from the stellar parameters. In general, the wind mass-loss rates decrease with decreasing metallicity and this relationship steepens for very low metallicities, Z less than or similar to 0.1 Z(circle dot). Down to metallicities corresponding to the Magellanic Clouds and even lower, the predicted mass-loss rates reasonably agree with observational estimates. However, the theoretical and observational mass-loss rates for very low metallicities exhibit significant scatter. We show that the scatter of observational values can be caused by inefficient shock cooling in the stellar wind, which leaves a considerable fraction of the wind at too high temperatures with waning observational signatures. The scatter of theoretical predictions is caused by a low number of lines that effectively accelerate the wind at very low metallicities.

Název v anglickém jazyce

New line-driven wind mass-loss rates for OB stars with metallicities down to 0.01 Z⊙

Popis výsledku anglicky

We provide new line-driven wind models for OB stars with metallicities down to 0.01 Z(circle dot). The models were calculated with our global wind code METUJE, which solves the hydrodynamical equations from nearly hydrostatic photosphere to supersonically expanding stellar wind together with the equations of statistical equilibrium and the radiative transfer equation. The models predict the basic wind parameters, namely, the wind mass-loss rates and terminal velocities just from the stellar parameters. In general, the wind mass-loss rates decrease with decreasing metallicity and this relationship steepens for very low metallicities, Z less than or similar to 0.1 Z(circle dot). Down to metallicities corresponding to the Magellanic Clouds and even lower, the predicted mass-loss rates reasonably agree with observational estimates. However, the theoretical and observational mass-loss rates for very low metallicities exhibit significant scatter. We show that the scatter of observational values can be caused by inefficient shock cooling in the stellar wind, which leaves a considerable fraction of the wind at too high temperatures with waning observational signatures. The scatter of theoretical predictions is caused by a low number of lines that effectively accelerate the wind at very low metallicities.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA25-15910S" target="_blank" >GA25-15910S: Větry horkých hvězd: řešení nejistot ztráty hmoty v blízkosti Eddingtonovy limity</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2025

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

1432-0746

Svazek periodika

702

Číslo periodika v rámci svazku

Sept.

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

11

Strana od-do

A9

Kód UT WoS článku

001582547500010

EID výsledku v databázi Scopus

2-s2.0-105017761430