EVOLUTION OF SUPER STAR CLUSTER WINDS WITH STRONG COOLING
We study the evolution of super star cluster winds driven by stellar winds and supernova explosions. Time-dependent rates at which mass and energy are deposited into the cluster volume, as well as the time-dependent chemical composition of the re-inserted gas, are obtained from the population synthe...
| Autores: | , |
|---|---|
| Tipo de documento: | artigo |
| Estado: | Versión aceptada para publicación |
| Data de publicação: | 2011 |
| País: | México |
| Recursos: | Instituto Nacional de Astrofísica, Óptica y Electrónica |
| Repositório: | Repositorio Institucional del INAOE |
| Idioma: | inglês |
| OAI Identifier: | oai:inaoe.repositorioinstitucional.mx:1009/1890 |
| Acesso em linha: | http://inaoe.repositorioinstitucional.mx/jspui/handle/1009/1890 |
| Access Level: | Acceso aberto |
| Palavra-chave: | info:eu-repo/classification/Inspec/Galaxies: star clusters: general info:eu-repo/classification/Inspec/HII regions info:eu-repo/classification/Inspec/ISM: bubbles info:eu-repo/classification/Inspec/ISM: general info:eu-repo/classification/cti/1 info:eu-repo/classification/cti/21 |
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EVOLUTION OF SUPER STAR CLUSTER WINDS WITH STRONG COOLINGSERGIY SILICHGUILLERMO TENORIO TAGLEinfo:eu-repo/classification/Inspec/Galaxies: star clusters: generalinfo:eu-repo/classification/Inspec/HII regionsinfo:eu-repo/classification/Inspec/ISM: bubblesinfo:eu-repo/classification/Inspec/ISM: generalinfo:eu-repo/classification/cti/1info:eu-repo/classification/cti/21info:eu-repo/classification/cti/21We study the evolution of super star cluster winds driven by stellar winds and supernova explosions. Time-dependent rates at which mass and energy are deposited into the cluster volume, as well as the time-dependent chemical composition of the re-inserted gas, are obtained from the population synthesis code Starburst99. These results are used as input for a semi-analytic code which determines the hydrodynamic properties of the cluster wind as a function of cluster age. Two types of winds are detected in the calculations. For the quasi-adiabatic solution, all of the inserted gas leaves the cluster in the form of a stationary wind. For the bimodal solution, some of the inserted gas becomes thermally unstable and forms dense warm clumps which accumulate inside the cluster. We calculate the evolution of the wind velocity and energy flux and integrate the amount of accumulated mass for clusters of different mass, radius, and initial metallicity. We also consider conditions with low heating efficiency of the re-inserted gas or mass loading of the hot thermalized plasma with the gas left over from star formation. We find that the bimodal regime and the related mass accumulation occur if at least one of the two conditions above is fulfilled.The Astrophysical Journal2011-10-20info:eu-repo/semantics/articleinfo:eu-repo/semantics/acceptedVersionapplication/pdfhttp://inaoe.repositorioinstitucional.mx/jspui/handle/1009/1890reponame:Repositorio Institucional del INAOEinstname:Instituto Nacional de Astrofísica, Óptica y Electrónicainstacron:INAOEengcitation:Wunsch, Richard., et al., (2011), EVOLUTION OF SUPER STAR CLUSTER WINDS WITH STRONG COOLING, The Astrophysical Journal, Vol. 740(75):1-7.info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-nd/4.0oai:inaoe.repositorioinstitucional.mx:1009/18902024-08-28T03:23:01Z |
| dc.title.none.fl_str_mv |
EVOLUTION OF SUPER STAR CLUSTER WINDS WITH STRONG COOLING |
| title |
EVOLUTION OF SUPER STAR CLUSTER WINDS WITH STRONG COOLING |
| spellingShingle |
EVOLUTION OF SUPER STAR CLUSTER WINDS WITH STRONG COOLING SERGIY SILICH info:eu-repo/classification/Inspec/Galaxies: star clusters: general info:eu-repo/classification/Inspec/HII regions info:eu-repo/classification/Inspec/ISM: bubbles info:eu-repo/classification/Inspec/ISM: general info:eu-repo/classification/cti/1 info:eu-repo/classification/cti/21 info:eu-repo/classification/cti/21 |
| title_short |
EVOLUTION OF SUPER STAR CLUSTER WINDS WITH STRONG COOLING |
| title_full |
EVOLUTION OF SUPER STAR CLUSTER WINDS WITH STRONG COOLING |
| title_fullStr |
EVOLUTION OF SUPER STAR CLUSTER WINDS WITH STRONG COOLING |
| title_full_unstemmed |
EVOLUTION OF SUPER STAR CLUSTER WINDS WITH STRONG COOLING |
| title_sort |
EVOLUTION OF SUPER STAR CLUSTER WINDS WITH STRONG COOLING |
| dc.creator.none.fl_str_mv |
SERGIY SILICH GUILLERMO TENORIO TAGLE |
| author |
SERGIY SILICH |
| author_facet |
SERGIY SILICH GUILLERMO TENORIO TAGLE |
| author_role |
author |
| author2 |
GUILLERMO TENORIO TAGLE |
| author2_role |
author |
| dc.subject.none.fl_str_mv |
info:eu-repo/classification/Inspec/Galaxies: star clusters: general info:eu-repo/classification/Inspec/HII regions info:eu-repo/classification/Inspec/ISM: bubbles info:eu-repo/classification/Inspec/ISM: general info:eu-repo/classification/cti/1 info:eu-repo/classification/cti/21 info:eu-repo/classification/cti/21 |
| topic |
info:eu-repo/classification/Inspec/Galaxies: star clusters: general info:eu-repo/classification/Inspec/HII regions info:eu-repo/classification/Inspec/ISM: bubbles info:eu-repo/classification/Inspec/ISM: general info:eu-repo/classification/cti/1 info:eu-repo/classification/cti/21 info:eu-repo/classification/cti/21 |
| description |
We study the evolution of super star cluster winds driven by stellar winds and supernova explosions. Time-dependent rates at which mass and energy are deposited into the cluster volume, as well as the time-dependent chemical composition of the re-inserted gas, are obtained from the population synthesis code Starburst99. These results are used as input for a semi-analytic code which determines the hydrodynamic properties of the cluster wind as a function of cluster age. Two types of winds are detected in the calculations. For the quasi-adiabatic solution, all of the inserted gas leaves the cluster in the form of a stationary wind. For the bimodal solution, some of the inserted gas becomes thermally unstable and forms dense warm clumps which accumulate inside the cluster. We calculate the evolution of the wind velocity and energy flux and integrate the amount of accumulated mass for clusters of different mass, radius, and initial metallicity. We also consider conditions with low heating efficiency of the re-inserted gas or mass loading of the hot thermalized plasma with the gas left over from star formation. We find that the bimodal regime and the related mass accumulation occur if at least one of the two conditions above is fulfilled. |
| publishDate |
2011 |
| dc.date.none.fl_str_mv |
2011-10-20 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/acceptedVersion |
| format |
article |
| status_str |
acceptedVersion |
| dc.identifier.none.fl_str_mv |
http://inaoe.repositorioinstitucional.mx/jspui/handle/1009/1890 |
| url |
http://inaoe.repositorioinstitucional.mx/jspui/handle/1009/1890 |
| dc.language.none.fl_str_mv |
eng |
| language |
eng |
| dc.relation.none.fl_str_mv |
citation:Wunsch, Richard., et al., (2011), EVOLUTION OF SUPER STAR CLUSTER WINDS WITH STRONG COOLING, The Astrophysical Journal, Vol. 740(75):1-7. |
| dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by-nc-nd/4.0 |
| eu_rights_str_mv |
openAccess |
| rights_invalid_str_mv |
http://creativecommons.org/licenses/by-nc-nd/4.0 |
| dc.format.none.fl_str_mv |
application/pdf |
| dc.publisher.none.fl_str_mv |
The Astrophysical Journal |
| publisher.none.fl_str_mv |
The Astrophysical Journal |
| dc.source.none.fl_str_mv |
reponame:Repositorio Institucional del INAOE instname:Instituto Nacional de Astrofísica, Óptica y Electrónica instacron:INAOE |
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Instituto Nacional de Astrofísica, Óptica y Electrónica |
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INAOE |
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INAOE |
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Repositorio Institucional del INAOE |
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Repositorio Institucional del INAOE |
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| repository.mail.fl_str_mv |
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15,811543 |