Wind Models of Massive Stars and Mass-Loss Rates Determination

Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F21%3A00552696" target="_blank" >RIV/67985815:_____/21:00552696 - isvavai.cz</a>
Result on the web
<a href="https://publications.aob.rs/100/pdf/107-114.pdf" target="_blank" >https://publications.aob.rs/100/pdf/107-114.pdf</a>
DOI - Digital Object Identifier
—

Result language
angličtina
Original language name
Wind Models of Massive Stars and Mass-Loss Rates Determination
Original language description
Determination of mass-loss rates of massive stars is an important output of massive star analysis, which influences our understanding of stellar evolution. Stellar mass-loss rates are usually determined using wind models with a different level of sophistication. Commonly used models are based on an assumption of spherical symmetry and solve the NLTE radiative transfer consistently for a given density and velocity structure, which means that the hydrodynamic structure is held fixed. Usually, an approximate dependence of velocity on radius is being assumed (the so-called β-velocity law). Using a different approach, mass-loss rates can be predicted by hydrodynamic models, which do not solve the radiative transfer, but they describe the radiation force in a parametric way (using force multipliers). The most sophisticated wind models do not use the simplifications of the β-velocity law and the force multlipliers. Consistent NLTE wind models including both the wind dynamics and NLTE radiative transfer can be calculated.
Czech name
—
Czech description
—

Project
—
Continuities
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year
2021
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Similar results(10)