Models of Solar and Stellar Atmospheres
Identifikátory výsledku
Kód výsledku v IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F19%3A00511176" target="_blank" >RIV/67985815:_____/19:00511176 - isvavai.cz</a>
Výsledek na webu
<a href="http://dx.doi.org/10.1016/B978-0-12-814334-6.00006-6" target="_blank" >http://dx.doi.org/10.1016/B978-0-12-814334-6.00006-6</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1016/B978-0-12-814334-6.00006-6" target="_blank" >10.1016/B978-0-12-814334-6.00006-6</a>
Alternativní jazyky
Jazyk výsledku
angličtina
Název v původním jazyce
Models of Solar and Stellar Atmospheres
Popis výsledku v původním jazyce
The chapter addresses the basic principles of the radiative transfer theory and nonequilibrium plasma physics, which were developed during the past century and are now widely used to model solar and stellar atmospheres. Many key results have been obtained and new numerical methods developed by solar physicists they serve as a guide for stellar astrophysics. We start with the basics of radiation transport and demonstrate the classical ideas of the nonequilibrium line formation using a two-level atom example. Then we summarize the equations used to construct standard plane-parallel models of atmospheres in hydrostatic and radiative equilibrium and show examples of models with different levels of complexity. Although such models are well-suited for modeling photospheres, solar and stellar chromospheres require even more advanced approaches. The simplest is represented by so-called semiempirical models. We show some classical examples for the Sun and cool stars. A specific class of problems concerns isolated atmospheric structures illuminated by solar or stellar disk radiation. Based on various atmospheric models, we discuss how model spectra are synthesized and spectral lines are actually formed. Finally, we briefly introduce the topic of radiation hydrodynamics as the most sophisticated tool for solar and stellar atmospheric modeling.nn
Název v anglickém jazyce
Models of Solar and Stellar Atmospheres
Popis výsledku anglicky
The chapter addresses the basic principles of the radiative transfer theory and nonequilibrium plasma physics, which were developed during the past century and are now widely used to model solar and stellar atmospheres. Many key results have been obtained and new numerical methods developed by solar physicists they serve as a guide for stellar astrophysics. We start with the basics of radiation transport and demonstrate the classical ideas of the nonequilibrium line formation using a two-level atom example. Then we summarize the equations used to construct standard plane-parallel models of atmospheres in hydrostatic and radiative equilibrium and show examples of models with different levels of complexity. Although such models are well-suited for modeling photospheres, solar and stellar chromospheres require even more advanced approaches. The simplest is represented by so-called semiempirical models. We show some classical examples for the Sun and cool stars. A specific class of problems concerns isolated atmospheric structures illuminated by solar or stellar disk radiation. Based on various atmospheric models, we discuss how model spectra are synthesized and spectral lines are actually formed. Finally, we briefly introduce the topic of radiation hydrodynamics as the most sophisticated tool for solar and stellar atmospheric modeling.nn
Klasifikace
Druh
C - Kapitola v odborné knize
CEP obor
—
OECD FORD obor
10308 - Astronomy (including astrophysics,space science)
Návaznosti výsledku
Projekt
<a href="/cs/project/GA16-17586S" target="_blank" >GA16-17586S: Třídimensionální modelování klidných slunečních protuberancí</a><br>
Návaznosti
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Ostatní
Rok uplatnění
2019
Kód důvěrnosti údajů
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Údaje specifické pro druh výsledku
Název knihy nebo sborníku
Sun as a guide to stellar physics
ISBN
9780128143346
Počet stran výsledku
27
Strana od-do
157-183
Počet stran knihy
522
Název nakladatele
Elsevier Science BV
Místo vydání
Amsterdam
Kód UT WoS kapitoly
—