Rayleigh scattering in the atmospheres of hot stars

J 2016

Rayleigh scattering in the atmospheres of hot stars

FIŠÁK, Jakub, Jiří KRTIČKA, Dominik MUNZAR a Jiří KUBÁT

Základní údaje

Originální název

Rayleigh scattering in the atmospheres of hot stars

Autoři

FIŠÁK, Jakub (203 Česká republika, domácí), Jiří KRTIČKA (203 Česká republika, domácí), Dominik MUNZAR (203 Česká republika, domácí) a Jiří KUBÁT (203 Česká republika)

Vydání

Astronomy & Astrophysics, 2016, 1432-0746

Další údaje

Jazyk

angličtina

Typ výsledku

Článek v odborném periodiku

Obor

10308 Astronomy

Stát vydavatele

Francie

Utajení

není předmětem státního či obchodního tajemství

Impakt faktor

Impact factor: 5.014

Kód RIV

RIV/00216224:14310/16:00090083

Organizační jednotka

Přírodovědecká fakulta

DOI

http://dx.doi.org/10.1051/0004-6361/201628291

UT WoS

000378106800118

Klíčová slova anglicky

atomic processes / scattering ; stars: chemically peculiar; stars: atmospheres; stars: early-type

Štítky

AKR, rivok

Příznaky

Mezinárodní význam, Recenzováno

Změněno: 10. 4. 2017 21:51, Ing. Andrea Mikešková

Anotace

V originále

Context. Rayleigh scattering is a result of an interaction of photons with bound electrons. Rayleigh scattering is mostly neglected in calculations of hot star model atmospheres because most of the hydrogen atoms are ionized and the heavier elements have a lower abundance than hydrogen. In atmospheres of some chemically peculiar stars, helium overabundant regions containing singly ionized helium are present and Rayleigh scattering can be a significant opacity source. Aims. We evaluate the contribution of Rayleigh scattering by neutral hydrogen and singly ionized helium in the atmospheres of hot stars with solar composition and in the atmospheres of helium overabundant stars. Methods. We computed several series of model atmospheres using the TLUSTY code and emergent fluxes using the SYNSPEC code. These models describe atmospheres of main sequence B-type stars with different helium abundance. We used an existing grid of models for atmospheres with solar chemical composition and we calculated an additional grid for helium-rich stars. Results. Rayleigh scattering by neutral hydrogen can be neglected in atmospheres of hot stars, while Rayleigh scattering by singly ionized helium can be a non-negligible opacity source in some hot stars, especially in helium-rich stars.

Citovat

FIŠÁK, Jakub, Jiří KRTIČKA, Dominik MUNZAR a Jiří KUBÁT. Rayleigh scattering in the atmospheres of hot stars. Astronomy & Astrophysics. 2016, roč. 590, June, s. "nestrankovano", 6 s. ISSN 1432-0746. Dostupné z: https://dx.doi.org/10.1051/0004-6361/201628291.

@article{1346555,
   author = {Fišák, Jakub and Krtička, Jiří and Munzar, Dominik and Kubát, Jiří},
   article_number = {June},
   doi = {http://dx.doi.org/10.1051/0004-6361/201628291},
   keywords = {atomic processes / scattering ; stars: chemically peculiar; stars: atmospheres; stars: early-type},
   language = {eng},
   issn = {1432-0746},
   journal = {Astronomy & Astrophysics},
   title = {Rayleigh scattering in the atmospheres of hot stars},
   volume = {590},
   year = {2016}
}

TY  - JOUR
ID  - 1346555
AU  - Fišák, Jakub - Krtička, Jiří - Munzar, Dominik - Kubát, Jiří
PY  - 2016
TI  - Rayleigh scattering in the atmospheres of hot stars
JF  - Astronomy & Astrophysics
VL  - 590
IS  - June
SP  - "nestrankovano"
EP  - "nestrankovano"
SN  - 14320746
KW  - atomic processes / scattering
KW  - stars: chemically peculiar
KW  - stars: atmospheres
KW  - stars: early-type
N2  - Context. Rayleigh scattering is a result of an interaction of photons with bound electrons. Rayleigh scattering is mostly neglected in calculations of hot star model atmospheres because most of the hydrogen atoms are ionized and the heavier elements have a lower abundance than hydrogen. In atmospheres of some chemically peculiar stars, helium overabundant regions containing singly ionized helium are present and Rayleigh scattering can be a significant opacity source. Aims. We evaluate the contribution of Rayleigh scattering by neutral hydrogen and singly ionized helium in the atmospheres of hot stars with solar composition and in the atmospheres of helium overabundant stars. Methods. We computed several series of model atmospheres using the TLUSTY code and emergent fluxes using the SYNSPEC code. These models describe atmospheres of main sequence B-type stars with different helium abundance. We used an existing grid of models for atmospheres with solar chemical composition and we calculated an additional grid for helium-rich stars. Results. Rayleigh scattering by neutral hydrogen can be neglected in atmospheres of hot stars, while Rayleigh scattering by singly ionized helium can be a non-negligible opacity source in some hot stars, especially in helium-rich stars.
ER  -

FIŠÁK, Jakub, Jiří KRTIČKA, Dominik MUNZAR a Jiří KUBÁT. Rayleigh scattering in the atmospheres of hot stars. \textit{Astronomy \&{} Astrophysics}. 2016, roč.~590, June, s.~''nestrankovano'', 6 s. ISSN~1432-0746. Dostupné z: https://dx.doi.org/10.1051/0004-6361/201628291.

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