What Physical Processes Drive the Interstellar Medium in the Local Bubble?
Autor(a) principal: | |
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Data de Publicação: | 2009 |
Outros Autores: | , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) |
Texto Completo: | http://hdl.handle.net/10174/5645 https://doi.org/10.1007/s11214-008-9425-1 |
Resumo: | Recent 3D high-resolution simulations of the interstellar medium in a star form- ing galaxy like the Milky Way show that supernova explosions are the main driver of the structure and evolution of the gas. Its physical state is largely controlled by turbulence due to the high Reynolds numbers of the average flows. For a constant supernova rate a dynam- ical equilibrium is established within 200 Myr of simulation as a consequence of the setup of a galactic fountain. The resulting interstellar medium reveals a typical density/pressure pattern, i.e. distribution of so-called gas phases, on scales of 500–700 pc, with interstellar bubbles being a common phenomenon just like the Local Bubble and the Loop I superbub- ble, which are assumed to be interacting. However, modeling the Local Bubble is special, because it is driven by a moving group, passing through its volume, as it is inferred from the analysis of Hipparcos data. A detailed analysis reveals that between 14 and 19 super- novae have exploded during the last 15 Myr. The age of the Local Bubble is derived from comparison with HI and UV absorption line data to be 14.5±0.7 Myr. We further predict the 0.4merging of the two bubbles in about 3 Myr from now, when the interaction shell starts to fragment. The Local Cloud and its companion HI clouds are the consequence of a dynamical instability in the interaction shell between the Local and the Loop I bubble. |
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What Physical Processes Drive the Interstellar Medium in the Local Bubble?Interstellar matterSuperbubblesLocal bubbleTurbulenceRecent 3D high-resolution simulations of the interstellar medium in a star form- ing galaxy like the Milky Way show that supernova explosions are the main driver of the structure and evolution of the gas. Its physical state is largely controlled by turbulence due to the high Reynolds numbers of the average flows. For a constant supernova rate a dynam- ical equilibrium is established within 200 Myr of simulation as a consequence of the setup of a galactic fountain. The resulting interstellar medium reveals a typical density/pressure pattern, i.e. distribution of so-called gas phases, on scales of 500–700 pc, with interstellar bubbles being a common phenomenon just like the Local Bubble and the Loop I superbub- ble, which are assumed to be interacting. However, modeling the Local Bubble is special, because it is driven by a moving group, passing through its volume, as it is inferred from the analysis of Hipparcos data. A detailed analysis reveals that between 14 and 19 super- novae have exploded during the last 15 Myr. The age of the Local Bubble is derived from comparison with HI and UV absorption line data to be 14.5±0.7 Myr. We further predict the 0.4merging of the two bubbles in about 3 Myr from now, when the interaction shell starts to fragment. The Local Cloud and its companion HI clouds are the consequence of a dynamical instability in the interaction shell between the Local and the Loop I bubble.Springer2012-11-15T14:57:02Z2012-11-152009-03-01T00:00:00Zinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articlehttp://hdl.handle.net/10174/5645http://hdl.handle.net/10174/5645https://doi.org/10.1007/s11214-008-9425-1eng263-276143Space Science Reviewsbreitschwerdt@astro.univie.ac.atmavillez@galaxy.lca.uevora.ptfuchs@ari.uni-heidelberg.dend343Breitschwerdt, Dieterde Avillez, MiguelFuchs, BurkhardDettbarn, Christianinfo:eu-repo/semantics/openAccessreponame:Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos)instname:Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informaçãoinstacron:RCAAP2024-01-03T18:44:40Zoai:dspace.uevora.pt:10174/5645Portal AgregadorONGhttps://www.rcaap.pt/oai/openaireopendoar:71602024-03-20T01:00:40.984885Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) - Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informaçãofalse |
dc.title.none.fl_str_mv |
What Physical Processes Drive the Interstellar Medium in the Local Bubble? |
title |
What Physical Processes Drive the Interstellar Medium in the Local Bubble? |
spellingShingle |
What Physical Processes Drive the Interstellar Medium in the Local Bubble? Breitschwerdt, Dieter Interstellar matter Superbubbles Local bubble Turbulence |
title_short |
What Physical Processes Drive the Interstellar Medium in the Local Bubble? |
title_full |
What Physical Processes Drive the Interstellar Medium in the Local Bubble? |
title_fullStr |
What Physical Processes Drive the Interstellar Medium in the Local Bubble? |
title_full_unstemmed |
What Physical Processes Drive the Interstellar Medium in the Local Bubble? |
title_sort |
What Physical Processes Drive the Interstellar Medium in the Local Bubble? |
author |
Breitschwerdt, Dieter |
author_facet |
Breitschwerdt, Dieter de Avillez, Miguel Fuchs, Burkhard Dettbarn, Christian |
author_role |
author |
author2 |
de Avillez, Miguel Fuchs, Burkhard Dettbarn, Christian |
author2_role |
author author author |
dc.contributor.author.fl_str_mv |
Breitschwerdt, Dieter de Avillez, Miguel Fuchs, Burkhard Dettbarn, Christian |
dc.subject.por.fl_str_mv |
Interstellar matter Superbubbles Local bubble Turbulence |
topic |
Interstellar matter Superbubbles Local bubble Turbulence |
description |
Recent 3D high-resolution simulations of the interstellar medium in a star form- ing galaxy like the Milky Way show that supernova explosions are the main driver of the structure and evolution of the gas. Its physical state is largely controlled by turbulence due to the high Reynolds numbers of the average flows. For a constant supernova rate a dynam- ical equilibrium is established within 200 Myr of simulation as a consequence of the setup of a galactic fountain. The resulting interstellar medium reveals a typical density/pressure pattern, i.e. distribution of so-called gas phases, on scales of 500–700 pc, with interstellar bubbles being a common phenomenon just like the Local Bubble and the Loop I superbub- ble, which are assumed to be interacting. However, modeling the Local Bubble is special, because it is driven by a moving group, passing through its volume, as it is inferred from the analysis of Hipparcos data. A detailed analysis reveals that between 14 and 19 super- novae have exploded during the last 15 Myr. The age of the Local Bubble is derived from comparison with HI and UV absorption line data to be 14.5±0.7 Myr. We further predict the 0.4merging of the two bubbles in about 3 Myr from now, when the interaction shell starts to fragment. The Local Cloud and its companion HI clouds are the consequence of a dynamical instability in the interaction shell between the Local and the Loop I bubble. |
publishDate |
2009 |
dc.date.none.fl_str_mv |
2009-03-01T00:00:00Z 2012-11-15T14:57:02Z 2012-11-15 |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
dc.type.driver.fl_str_mv |
info:eu-repo/semantics/article |
format |
article |
status_str |
publishedVersion |
dc.identifier.uri.fl_str_mv |
http://hdl.handle.net/10174/5645 http://hdl.handle.net/10174/5645 https://doi.org/10.1007/s11214-008-9425-1 |
url |
http://hdl.handle.net/10174/5645 https://doi.org/10.1007/s11214-008-9425-1 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
263-276 143 Space Science Reviews breitschwerdt@astro.univie.ac.at mavillez@galaxy.lca.uevora.pt fuchs@ari.uni-heidelberg.de nd 343 |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.publisher.none.fl_str_mv |
Springer |
publisher.none.fl_str_mv |
Springer |
dc.source.none.fl_str_mv |
reponame:Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) instname:Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informação instacron:RCAAP |
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Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informação |
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RCAAP |
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RCAAP |
reponame_str |
Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) |
collection |
Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) |
repository.name.fl_str_mv |
Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) - Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informação |
repository.mail.fl_str_mv |
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1799136489964044288 |