Hot star wind models with new solar abundances

J 2007

Hot star wind models with new solar abundances

KRTIČKA, Jiří a Jiří KUBÁT

Základní údaje

Originální název

Hot star wind models with new solar abundances

Název česky

Modely hvězdných větrů horkých hvězd s novým slunečním chemickým složením

Autoři

KRTIČKA, Jiří a Jiří KUBÁT

Vydání

Astronomy and Astrophysics, Les Ulis Cedex, France, EDP Sciences, 2007, 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

Odkazy

URL

Impakt faktor

Impact factor: 4.259

Kód RIV

RIV/00216224:14310/07:00020178

Organizační jednotka

Přírodovědecká fakulta

UT WoS

000244679500004

Klíčová slova anglicky

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

Příznaky

Mezinárodní význam, Recenzováno

Změněno: 10. 4. 2012 14:48, prof. Mgr. Jiří Krtička, Ph.D.

Anotace

ORIG CZ

V originále

We compare the hot-star wind models calculated by assuming older solar-abundance determination with models calculated using the recently published values derived from 3D hydrodynamical model atmospheres. We show that the use of new abundances with lower metallicity improves the agreement between wind observation and theory in several aspects. (1) The predicted wind mass-loss rates are lower by a factor of 0.76. This leads to better agreement with mass-loss rates derived from observational analysis that takes the clumping into account. (2) As a result of the lowering of mass-loss rates, there is better agreement between the predicted modified wind momentum-luminosity relationship and that derived from observational analysis that takes the clumping into account. (3) Both the lower mass fraction of heavier elements and lower mass-loss rates lead to a decrease in opacity in the X-ray region. This influences the prediction of the X-ray line profile shapes. (4) There is better agreement between predicted PV ionization fractions and those derived from observations.

Česky

Porovnáváme modely hvězdných větrů horkých hvězd spočtené pomocí staršího určení chemického složení Slunce a nového určení chemického složení pomocí 3D hydrodynamických modelů atmosféry. Ukazujeme, že použití nového chemického složení s menším obsahem těžších prvků vylepšuje soulad mezi pozorováním a teorií v několika ohledech.

Návaznosti

GA205/04/1267, projekt VaV

Název: Okolohvězdné obálky horkých hvězd

Investor: Grantová agentura ČR, Okolohvězdné obálky horkých hvězd

Citovat

KRTIČKA, Jiří a Jiří KUBÁT. Hot star wind models with new solar abundances. Astronomy and Astrophysics. Les Ulis Cedex, France: EDP Sciences, 2007, roč. 2007, č. 464, s. L17-L20, 4 s. ISSN 0004-6361.

@article{713627,
   author = {Krtička, Jiří and Kubát, Jiří},
   article_location = {Les Ulis Cedex, France},
   article_number = {464},
   keywords = {stars: winds outflows - stars: mass-loss - stars: early-type - hydrodynamics},
   language = {eng},
   issn = {0004-6361},
   journal = {Astronomy and Astrophysics},
   title = {Hot star wind models with new solar abundances},
   url = {http://www.aanda.org/index.php?option=com_base_ora&access=standard&Itemid=129&url=articles/aa/abs/2007/11/aa6775-06/aa6775-06.html},
   volume = {2007},
   year = {2007}
}

TY  - JOUR
ID  - 713627
AU  - Krtička, Jiří - Kubát, Jiří
PY  - 2007
TI  - Hot star wind models with new solar abundances
JF  - Astronomy and Astrophysics
VL  - 2007
IS  - 464
SP  - L17-L20
EP  - L17-L20
PB  - EDP Sciences
SN  - 00046361
KW  - stars: winds outflows  - stars: mass-loss  - stars: early-type  - hydrodynamics
UR  - http://www.aanda.org/index.php?option=com_base_ora&access=standard&Itemid=129&url=articles/aa/abs/2007/11/aa6775-06/aa6775-06.html
N2  - We compare the hot-star wind models calculated by assuming older solar-abundance determination with models calculated using the recently published values derived from 3D hydrodynamical model atmospheres. We show that the use of new abundances with lower metallicity improves the agreement between wind observation and theory in several aspects. (1) The predicted wind mass-loss rates are lower by a factor of 0.76. This leads to better agreement with mass-loss rates derived from observational analysis that takes the clumping into account. (2) As a result of the lowering of mass-loss rates, there is better agreement between the predicted modified wind momentum-luminosity relationship and that derived from observational analysis that takes the clumping into account. (3) Both the lower mass fraction of heavier elements and lower mass-loss rates lead to a decrease in opacity in the X-ray region. This influences the prediction of the X-ray line profile shapes. (4) There is better agreement between predicted PV ionization fractions and those derived from observations.
ER  -

KRTIČKA, Jiří a Jiří KUBÁT. Hot star wind models with new solar abundances. \textit{Astronomy and Astrophysics}. Les Ulis Cedex, France: EDP Sciences, 2007, roč.~2007, č.~464, s.~L17-L20, 4 s. ISSN~0004-6361.

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