Disk formation in hierarchical hydrodynamical simulations: A way out of the angular momentum catastrophe

We report results on the formation of disklike structures in two cosmological hydrodynamical simulations, which share the same initial conditions, in a hierarchical clustering scenario. In the first simulation, a simple and generic implementation of star formation has allowed galaxy-like objects wit...

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Detalles Bibliográficos
Publicado: 1998
Materias:
Cosmology: observations
Cosmology: theory
Dark matter
Galaxies: formation
Methods: numerical
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v508_n2PARTII_pL123_DominguezTenreiro
http://hdl.handle.net/20.500.12110/paper_0004637X_v508_n2PARTII_pL123_DominguezTenreiro
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_0004637X_v508_n2PARTII_pL123_DominguezTenreiro
record_format dspace
spelling paper:paper_0004637X_v508_n2PARTII_pL123_DominguezTenreiro2023-06-08T14:28:40Z Disk formation in hierarchical hydrodynamical simulations: A way out of the angular momentum catastrophe Cosmology: observations Cosmology: theory Dark matter Galaxies: formation Methods: numerical We report results on the formation of disklike structures in two cosmological hydrodynamical simulations, which share the same initial conditions, in a hierarchical clustering scenario. In the first simulation, a simple and generic implementation of star formation has allowed galaxy-like objects with stellar bulges and extended, populated disks to form. Gas in the disk comes both from particles that survive mergers, keeping in part their angular momentum content, and from new gas supplied by infall once the merger process is over, with global specific angular momentum conservation. The stellar bulge forms from gas that has lost most of its angular momentum. In the second simulation, no star formation has been included. In this case, objects consist of an overpopulated central gas concentration and an extended, underpopulated disk. The central concentration forms from particles that suffer an important angular momentum loss in violent events, and it often contains more than 70% of the object's baryonic mass. The external disk forms by late infall of gas that roughly conserves its specific angular momentum. The difference between these two simulations is likely to be due to the stabilizing character of the stellar bulge-like cores that form in the first simulation, which diminishes the inflow of gas triggered by mergers and interactions. © 1998. The American Astronomical Society. All rights reserved. 1998 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v508_n2PARTII_pL123_DominguezTenreiro http://hdl.handle.net/20.500.12110/paper_0004637X_v508_n2PARTII_pL123_DominguezTenreiro
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Cosmology: observations
Cosmology: theory
Dark matter
Galaxies: formation
Methods: numerical
spellingShingle Cosmology: observations
Cosmology: theory
Dark matter
Galaxies: formation
Methods: numerical
Disk formation in hierarchical hydrodynamical simulations: A way out of the angular momentum catastrophe
topic_facet Cosmology: observations
Cosmology: theory
Dark matter
Galaxies: formation
Methods: numerical
description We report results on the formation of disklike structures in two cosmological hydrodynamical simulations, which share the same initial conditions, in a hierarchical clustering scenario. In the first simulation, a simple and generic implementation of star formation has allowed galaxy-like objects with stellar bulges and extended, populated disks to form. Gas in the disk comes both from particles that survive mergers, keeping in part their angular momentum content, and from new gas supplied by infall once the merger process is over, with global specific angular momentum conservation. The stellar bulge forms from gas that has lost most of its angular momentum. In the second simulation, no star formation has been included. In this case, objects consist of an overpopulated central gas concentration and an extended, underpopulated disk. The central concentration forms from particles that suffer an important angular momentum loss in violent events, and it often contains more than 70% of the object's baryonic mass. The external disk forms by late infall of gas that roughly conserves its specific angular momentum. The difference between these two simulations is likely to be due to the stabilizing character of the stellar bulge-like cores that form in the first simulation, which diminishes the inflow of gas triggered by mergers and interactions. © 1998. The American Astronomical Society. All rights reserved.
title Disk formation in hierarchical hydrodynamical simulations: A way out of the angular momentum catastrophe
title_short Disk formation in hierarchical hydrodynamical simulations: A way out of the angular momentum catastrophe
title_full Disk formation in hierarchical hydrodynamical simulations: A way out of the angular momentum catastrophe
title_fullStr Disk formation in hierarchical hydrodynamical simulations: A way out of the angular momentum catastrophe
title_full_unstemmed Disk formation in hierarchical hydrodynamical simulations: A way out of the angular momentum catastrophe
title_sort disk formation in hierarchical hydrodynamical simulations: a way out of the angular momentum catastrophe
publishDate 1998
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v508_n2PARTII_pL123_DominguezTenreiro
http://hdl.handle.net/20.500.12110/paper_0004637X_v508_n2PARTII_pL123_DominguezTenreiro
_version_ 1768544891892137984

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