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Star Formation Efficiency in Low-Density Regions in Galactic Disksстатья
Информация о цитировании статьи получена из
Web of Science,
Scopus
Статья опубликована в журнале из списка Web of Science и/или Scopus
Дата последнего поиска статьи во внешних источниках: 19 июля 2013 г.
- Авторы: Abramova O.V., Zasov A.V.
- Журнал: Astronomy Letters
- Том: 38
- Номер: 12
- Год издания: 2012
- Издательство: Maik Nauka/Interperiodica Publishing
- Местоположение издательства: Russian Federation
- Первая страница: 755
- Последняя страница: 763
- DOI: 10.1134/S1063773712120018
- Аннотация: The radial dependences of the star formation efficiency ΣSFE = ΣSFR/Σgas (per unit disk surface area) in normal surface brightness spiral galaxies and low surface brightness (LSB) galaxies are compared with the radial variations of the gas and stellar disk surface and volume densities. The volume density of the components in the disk midplane is found through a self-consistent solution of the disk equilibrium equations by taking into account the dark halo. The disk thickness variation with radius R is calculated within the model of a galaxy with a marginally stable disk by taking into account the increase stability parameter QT,c along the radius. We show that the star formation efficiency depends weakly (for LSB galaxies, does not depend at all) on the gas density but correlates well with the disk surface and volume density, with the normal and LSB galaxies forming a single sequence. The dependence vanishes only at extremely low disk densities (σdisk ≤ (1−3) M pc−2, ρstars ≤ (1−3) × 10−24 g cm−3), where star formation probably ceases to be related to disk properties. Estimations of the gas volume density allow us to check the expected form of the ΣSFR–σdisk relationship that follows from the model by Ostriker et al., which relates the star formation rate to the pressure of the diffuse gas medium. For most of the galaxies considered, there is satisfactory agreement with the model, except for the densest (of the order of several hundredM pc−2) and least dense (severalM pc−2 or less) disk regions.
- Добавил в систему: Абрамова Оксана Викторовна