The Effects on a Core Collapse of Changes in the Number and Size of Turbulent Modes of Velocity

The Effects on a Core Collapse of Changes in the Number and Size of Turbulent Modes of Velocity

ABSTRACT We consider 28 particle-based simulations aimed at comparing the gravitational collapse of a spherically symmetric, uniform gas core in which two extreme types of turbulent spectra of velocity have been initially induced, so that ∇ ν → = 0 (14 simulations) and ∇× ν → = 0 (14 simulations). For all the simulations, the ratios of the kinetic energy and thermal energy to the gravitational energy were fixed at β=0.21 and α=0.24, respectively. Most of the simulations finish by forming a single protostar, except for two simulations that form a binary system of protostars. In order to quantify the differences (or similarities) between the two types of simulations, we calculate some integral properties of the resulting protostars, such as the mass Mf and the ratios αf and βf.

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Main Author: Arreaga-García,Guillermo
Format: Digital revista
Language:English
Published: Universidad Nacional Autónoma de México, Instituto de Astronomía 2017
Online Access:http://www.scielo.org.mx/scielo.php?script=sci_arttext&pid=S0185-11012017000200015
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spelling oai:scielo:S0185-110120170002000152019-10-21The Effects on a Core Collapse of Changes in the Number and Size of Turbulent Modes of VelocityArreaga-García,Guillermo hydrodynamics methods numerical stars formation turbulence ABSTRACT We consider 28 particle-based simulations aimed at comparing the gravitational collapse of a spherically symmetric, uniform gas core in which two extreme types of turbulent spectra of velocity have been initially induced, so that ∇ ν → = 0 (14 simulations) and ∇× ν → = 0 (14 simulations). For all the simulations, the ratios of the kinetic energy and thermal energy to the gravitational energy were fixed at β=0.21 and α=0.24, respectively. Most of the simulations finish by forming a single protostar, except for two simulations that form a binary system of protostars. In order to quantify the differences (or similarities) between the two types of simulations, we calculate some integral properties of the resulting protostars, such as the mass Mf and the ratios αf and βf.info:eu-repo/semantics/openAccessUniversidad Nacional Autónoma de México, Instituto de AstronomíaRevista mexicana de astronomía y astrofísica v.53 n.2 20172017-01-01info:eu-repo/semantics/articletext/htmlhttp://www.scielo.org.mx/scielo.php?script=sci_arttext&pid=S0185-11012017000200015en
institution SCIELO
collection OJS
country México
countrycode MX
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access En linea
databasecode rev-scielo-mx
tag revista
region America del Norte
libraryname SciELO
language English
format Digital
author Arreaga-García,Guillermo
spellingShingle Arreaga-García,Guillermo
The Effects on a Core Collapse of Changes in the Number and Size of Turbulent Modes of Velocity
author_facet Arreaga-García,Guillermo
author_sort Arreaga-García,Guillermo
title The Effects on a Core Collapse of Changes in the Number and Size of Turbulent Modes of Velocity
title_short The Effects on a Core Collapse of Changes in the Number and Size of Turbulent Modes of Velocity
title_full The Effects on a Core Collapse of Changes in the Number and Size of Turbulent Modes of Velocity
title_fullStr The Effects on a Core Collapse of Changes in the Number and Size of Turbulent Modes of Velocity
title_full_unstemmed The Effects on a Core Collapse of Changes in the Number and Size of Turbulent Modes of Velocity
title_sort effects on a core collapse of changes in the number and size of turbulent modes of velocity
description ABSTRACT We consider 28 particle-based simulations aimed at comparing the gravitational collapse of a spherically symmetric, uniform gas core in which two extreme types of turbulent spectra of velocity have been initially induced, so that ∇ ν → = 0 (14 simulations) and ∇× ν → = 0 (14 simulations). For all the simulations, the ratios of the kinetic energy and thermal energy to the gravitational energy were fixed at β=0.21 and α=0.24, respectively. Most of the simulations finish by forming a single protostar, except for two simulations that form a binary system of protostars. In order to quantify the differences (or similarities) between the two types of simulations, we calculate some integral properties of the resulting protostars, such as the mass Mf and the ratios αf and βf.
publisher Universidad Nacional Autónoma de México, Instituto de Astronomía
publishDate 2017
url http://www.scielo.org.mx/scielo.php?script=sci_arttext&pid=S0185-11012017000200015
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