Star Formation in Isolated Disk Galaxies. I. Models and Characteristics of Nonlinear Gravitational Collapse

We model gravitational collapse leading to star formation in a wide range of isolated disk galaxies using a three-dimensional, smoothed particle hydrodynamics code. The model galaxies include a dark matter halo and a disk of stars and isothermal gas. Absorbing sink particles are used to directly mea...

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Published inThe Astrophysical journal Vol. 626; no. 2; pp. 823 - 843
Main Authors Li, Yuexing, Mac Low, Mordecai-Mark, Klessen, Ralf S
Format Journal Article
LanguageEnglish
Published Chicago, IL IOP Publishing 20.06.2005
University of Chicago Press
Subjects
Galaxy evolution
galaxies: evolution
Disk galaxies
galaxies: star clusters
Star clusters
Galaxy clusters
stars: formation
Star formation
Dynamics
galaxies: ISM
Kinematics
Gravitational collapse
Models
Spiral galaxies
galaxies: kinematics and dynamics
galaxies: spiral
Online AccessGet full text

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Abstract We model gravitational collapse leading to star formation in a wide range of isolated disk galaxies using a three-dimensional, smoothed particle hydrodynamics code. The model galaxies include a dark matter halo and a disk of stars and isothermal gas. Absorbing sink particles are used to directly measure the mass of gravitationally collapsing gas. They reach masses characteristic of stellar clusters. In this paper we describe our galaxy models and numerical methods, followed by an investigation of the gravitational instability in these galaxies. Gravitational collapse forms star clusters with correlated positions and ages, as observed, for example, in the Large Magellanic Cloud. Gravitational instability alone acting in unperturbed galaxies appears sufficient to produce flocculent spiral arms, although not more organized patterns. Unstable galaxies show collapse in thin layers in the galactic plane; associated dust will form thin dust lanes in those galaxies, in agreement with observations. We find an exponential relationship between the global collapse timescale and the minimum value in a galaxy of the Toomre instability parameter for a combination of stars and gas Q sub(sg). Furthermore, collapse occurs only in regions with Q sub(sg) < 1.6. Our results suggest that vigorous starbursts occur where Q sub(sg) << 1, while slow star formation takes place at higher values of Q sub(sg) below 1.6. A massive, or gas-rich, galaxy has low initial Q sub(sg), giving it a high star formation rate, while a low-mass, or gas-poor, galaxy has a high initial Q sub(sg), giving it a low star formation rate.
AbstractList We model gravitational collapse leading to star formation in a wide range of isolated disk galaxies using a three-dimensional, smoothed particle hydrodynamics code. The model galaxies include a dark matter halo and a disk of stars and isothermal gas. Absorbing sink particles are used to directly measure the mass of gravitationally collapsing gas. They reach masses characteristic of stellar clusters. In this paper we describe our galaxy models and numerical methods, followed by an investigation of the gravitational instability in these galaxies. Gravitational collapse forms star clusters with correlated positions and ages, as observed, for example, in the Large Magellanic Cloud. Gravitational instability alone acting in unperturbed galaxies appears sufficient to produce flocculent spiral arms, although not more organized patterns. Unstable galaxies show collapse in thin layers in the galactic plane; associated dust will form thin dust lanes in those galaxies, in agreement with observations. We find an exponential relationship between the global collapse timescale and the minimum value in a galaxy of the Toomre instability parameter for a combination of stars and gas Q sub(sg). Furthermore, collapse occurs only in regions with Q sub(sg) < 1.6. Our results suggest that vigorous starbursts occur where Q sub(sg) << 1, while slow star formation takes place at higher values of Q sub(sg) below 1.6. A massive, or gas-rich, galaxy has low initial Q sub(sg), giving it a high star formation rate, while a low-mass, or gas-poor, galaxy has a high initial Q sub(sg), giving it a low star formation rate.
Author Li, Yuexing
Klessen, Ralf S
Mac Low, Mordecai-Mark
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Issue 2
Keywords Galaxy evolution
galaxies: evolution
Disk galaxies
galaxies: star clusters
Star clusters
Galaxy clusters
stars: formation
Star formation
Dynamics
galaxies: ISM
Kinematics
Gravitational collapse
Models
Spiral galaxies
galaxies: kinematics and dynamics
galaxies: spiral
Language English
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Snippet We model gravitational collapse leading to star formation in a wide range of isolated disk galaxies using a three-dimensional, smoothed particle hydrodynamics...
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Title Star Formation in Isolated Disk Galaxies. I. Models and Characteristics of Nonlinear Gravitational Collapse
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