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Journal ArticleDOI

Modeling of the Initial Mass Function Using the Metropolis−Hastings Algorithm

TLDR
In this article, a stochastic model for the hierarchical fragmentation of a molecular cloud was developed, where the number of fragments, time between successive fragmentation steps, and mass of a fragment were considered as random variables, and fragment masses were generated using the Metropolis-Hastings algorithm.
Abstract
A stochastic model has been developed for the hierarchical fragmentation of a molecular cloud. Here, the number of fragments, time between successive fragmentation steps, and mass of a fragment are considered as random variables, and fragment masses are generated using the Metropolis-Hastings algorithm. The resulting mass spectra, computed at different projected distances and taking opacity into consideration, show a signature of mass segregation. The critical mass, mass spectrum, and mass segregation are consistent with the observations of young massive clusters in our Galaxy as well as in external galaxies.

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Citations
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Journal ArticleDOI

The initial mass function modeled by a left truncated beta distribution

TL;DR: In this article, a left truncated beta probability density function was introduced to demonstrate the advantage of introducing a four-parameter initial mass function for the stars and the presence of brown dwarfs.
Journal ArticleDOI

Cosmic history of integrated galactic stellar initial mass function : a simulation study

TL;DR: In this paper, the authors investigated the effect of the evolution of the stellar initial mass function (IMF) with increasing redshift on the formation of massive clusters in star burst galaxies.
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Cosmic History of the Integrated Galactic Stellar Initial Mass Function: A Simulation Study

TL;DR: In this article, the authors investigate the evolution of the stellar initial mass function (IMF) and varying indices of β for the integrated galactic initial mass functions, in relation to several measures of star formation rates of galaxies at various redshifts by random simulation.
Journal ArticleDOI

The low-mass Initial Mass Function in the 30 Doradus starburst cluster

TL;DR: In this article, the authors presented deep Hubble Space Telescope (HST) NICMOS 2 F160W band observations of the central 56*57" (14pc*14.25pc) region around R136 in the starburst cluster 30 Dor (NGC 2070) located in the Large Magellanic Cloud.
Journal Article

The Formation and Early Dynamical Evolution of Bound Stellar Systems

TL;DR: In this paper, the results of numerical N-body calculations which simulate the dynamical evolution of young clusters as they emerge from molecular clouds have been presented, and the combination of these parameters which result in the production of bound stellar groups after the gas not used in star formation is completely dispersed.
References
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Journal ArticleDOI

Young star clusters in interacting galaxies - NGC 1487 and NGC 4038/4039

TL;DR: In this article, the dynamical masses of several young (≈10 Myr) massive star clusters in two interacting galaxies, NGC 4038/4039 (The Antennae) and NGC 1487, under the assumption of virial equilibrium were estimated.
Journal ArticleDOI

An HST/WFPC2 Survey of Bright Young Clusters in M31 III. Structural Parameters

TL;DR: In this paper, surface brightness profiles for 23 M31 star clusters were measured using images from the Wide Field Planetary Camera 2 on the Hubble Space Telescope, and fit to two types of models to determine the clusters' structural properties.
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A hubble space telescope/wfpc2 survey of bright young clusters in m31. iii. structural parameters*

TL;DR: In this article, surface brightness profiles for 23 M31 star clusters were measured using images from the Wide Field Planetary Camera 2 on the Hubble Space Telescope, and fitted to two types of models to determine the clusters' structural properties.
Journal ArticleDOI

The fragmentation of proto-globular clusters. I. Thermal instabilities

TL;DR: In this article, the authors assume that the fragmentation of a proto-globular cluster cloud proceeded in two steps, in the first step thermal instability led to the rapid growth of initial fluctuations, and the perturbations then underwent gravitational instabilities on short time scales.
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