Multicomponent radiatively driven stellar windsII.
Gayley-Owocki heating in multitemperature winds of OB stars

J 2001

Multicomponent radiatively driven stellar windsII. Gayley-Owocki heating in multitemperature winds of OB stars

KRTIČKA, Jiří a Jiří KUBÁT

Základní údaje

Originální název

Multicomponent radiatively driven stellar windsII. Gayley-Owocki heating in multitemperature winds of OB stars

Autoři

KRTIČKA, Jiří (203 Česká republika, garant) a Jiří KUBÁT

Vydání

Astronomy and Astrophysics, Les Ulis Cedex, France, EDP Sciences, 2001, 0004-6361

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: 2.790 v roce 2000

Kód RIV

RIV/00216224:14310/01:00004405

Organizační jednotka

Přírodovědecká fakulta

Klíčová slova anglicky

hydrodynamics -- stars: mass-loss -- stars: early-type -- stars: winds; outflows

Štítky

outflows

Příznaky

Mezinárodní význam, Recenzováno

Změněno: 5. 3. 2007 17:58, prof. Mgr. Jiří Krtička, Ph.D.

Anotace

V originále

We show that the so-called Gayley-Owocki (Doppler) heating is important for the temperature structure of the wind of main sequence stars cooler than the spectral type O6. The formula for Gayley-Owocki heating is derived directly from the Boltzmann equation as a direct consequence of the dependence of the driving force on the velocity gradient. Since Gayley-Owocki heating deposits heat directly on the absorbing ions, we also investigated the possibility that individual components of the radiatively driven stellar wind have different temperatures. This effect is negligible in the wind of O stars, whereas a significant temperature difference takes place in the winds of main sequence B stars for stars cooler than B2. Typical temperature differences between absorbing ions and other flow components for such stars is of the order 103 K. However, in the case when the passive component falls back onto the star, the absorbing component reaches temperatures of order 106 K, which allows for emission of X-rays. Moreover, we compare our computed terminal velocities with the observed ones. We found quite good agreement between predicted and observed terminal velocities. The systematic difference coming from the using of the so called "cooking formula" has been removed.

Návaznosti

GA205/01/0656, projekt VaV

Název: Modelování rozsáhlých obálek horkých hvězd

Citovat

KRTIČKA, Jiří a Jiří KUBÁT. Multicomponent radiatively driven stellar windsII. Gayley-Owocki heating in multitemperature winds of OB stars. Astronomy and Astrophysics. Les Ulis Cedex, France: EDP Sciences, 2001, roč. 35, č. 377, s. 175-191. ISSN 0004-6361.

@article{368252,
   author = {Krtička, Jiří and Kubát, Jiří},
   article_location = {Les Ulis Cedex, France},
   article_number = {377},
   keywords = {hydrodynamics -- stars: mass-loss -- stars: early-type -- stars: winds; outflows},
   language = {eng},
   issn = {0004-6361},
   journal = {Astronomy and Astrophysics},
   title = {Multicomponent radiatively driven stellar windsII. Gayley-Owocki heating in multitemperature winds of OB stars},
   volume = {35},
   year = {2001}
}

TY  - JOUR
ID  - 368252
AU  - Krtička, Jiří - Kubát, Jiří
PY  - 2001
TI  - Multicomponent radiatively driven stellar windsII. Gayley-Owocki heating in multitemperature winds of OB stars
JF  - Astronomy and Astrophysics
VL  - 35
IS  - 377
SP  - 175
EP  - 175
PB  - EDP Sciences
SN  - 00046361
KW  - hydrodynamics -- stars: mass-loss -- stars: early-type -- stars: winds
KW  - outflows
N2  - We show that the so-called Gayley-Owocki (Doppler) heating is important for the temperature structure of the wind of main sequence stars cooler than the spectral type O6. The formula for Gayley-Owocki heating is derived directly from the Boltzmann equation as a direct consequence of the dependence of the driving force on the velocity gradient. Since Gayley-Owocki heating deposits heat directly on the absorbing ions, we also investigated the possibility that individual components of the radiatively driven stellar wind have different temperatures. This effect is negligible in the wind of O stars, whereas a significant temperature difference takes place in the winds of main sequence B stars for stars cooler than B2. Typical temperature differences between absorbing ions and other flow components for such stars is of the order 103 K. However, in the case when the passive component falls back onto the star, the absorbing component reaches temperatures of order 106 K, which allows for emission of X-rays. Moreover, we compare our computed terminal velocities with the observed ones. We found quite good agreement between predicted and observed terminal velocities. The systematic difference coming from the using of the so called "cooking formula" has been removed.
ER  -

KRTIČKA, Jiří a Jiří KUBÁT. Multicomponent radiatively driven stellar windsII. Gayley-Owocki heating in multitemperature winds of OB stars. \textit{Astronomy and Astrophysics}. Les Ulis Cedex, France: EDP Sciences, 2001, roč.~35, č.~377, s.~175-191. ISSN~0004-6361.

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