Hot star wind models with new solar abundances

KRTIČKA, Jiří and Jiří KUBÁT. Hot star wind models with new solar abundances. Astronomy and Astrophysics. Les Ulis Cedex, France: EDP Sciences, 2007, vol. 2007, No 464, p. L17-L20, 4 pp. ISSN 0004-6361.

Basic information

• Original name: Hot star wind models with new solar abundances
• Name in Czech: Modely hvězdných větrů horkých hvězd s novým slunečním chemickým složením
• Authors: KRTIČKA, Jiří (203 Czech Republic, guarantor) and Jiří KUBÁT (203 Czech Republic).
• Edition: Astronomy and Astrophysics, Les Ulis Cedex, France, EDP Sciences, 2007, 0004-6361.

Other information

• Original language: English
• Type of outcome: Article in a journal
• Field of Study: 10308 Astronomy
• Country of publisher: France
• Confidentiality degree: is not subject to a state or trade secret
• WWW: URL
• Impact factor: Impact factor: 4.259
• RIV identification code: RIV/00216224:14310/07:00020178
• Organization unit: Faculty of Science
• UT WoS: 000244679500004
• Keywords in English: stars: winds outflows - stars: mass-loss - stars: early-type - hydrodynamics
• Tags: International impact, Reviewed

Abstract

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.

Abstract (in Czech)

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.

Links

• GA205/04/1267, research and development project: Name: Okolohvězdné obálky horkých hvězd

Investor: Czech Science Foundation, Circumstellar envelopes of hot stars