Chemodynamics of Star-Forming Regions

Autores
Hägele, Guillermo Federico; Firpo, Verónica; Bosch, Guillermo Luis; Díaz, Ángeles I.; Morrell, Nidia Irene; Campuzano Castro, Federico; Cardaci, Mónica Viviana
Año de publicación
2016
Idioma
inglés
Tipo de recurso
documento de conferencia
Estado
versión publicada
Descripción
The large number of massive stars belonging to regions with violent star formation dominates the morphology of the gas, the evolution of the different generations of stars and the physical conditions of their surrounding gaseous nebulae through the photoionization of the gas, strong stellar winds, super-bubble formation and material flows. The analysis of these processes between a starburst and its environment requires the complete study of the gaseous component, from its kinematical structure to its physical properties. Using different observational techniques, low-inter mediate and high-spectral resolution spectroscopy, the physical conditions (electron density and temperatures), ionic and total chemical abundances of several atoms, reddening and ionization, structure, for the global flux and for the different kinematical components can be derive. Applying the direct method or empirical relationships for abundance determination, wc are able to perform a comparative analysis between different star-forming regions belonging to the same galaxy. The relative abundances of N/O, S/O, Ne/O and Ar/O for the different kinematical components give us clues for a common or very similar chemical evolution for the different kinematical components of each knot. It could also be indicative that the different kinematical components are different phases of the same gas. Similarities between the ionization structure of the different kinematical components could imply that the effective temperatures of the ionizing radiation fields are very similar for all the components, in spite of some small differences in the ionization state of different elements. The ionizing star clusters that excite the gas associated, to each star-forming knot that produces the different kinematical components could therefore be the same.
Instituto de Astrofísica de La Plata
Materia
Ciencias Astronómicas
star-forming regions
chemical evolution
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/165640
Acceder
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spelling Chemodynamics of Star-Forming RegionsHägele, Guillermo FedericoFirpo, VerónicaBosch, Guillermo LuisDíaz, Ángeles I.Morrell, Nidia IreneCampuzano Castro, FedericoCardaci, Mónica VivianaCiencias Astronómicasstar-forming regionschemical evolutionThe large number of massive stars belonging to regions with violent star formation dominates the morphology of the gas, the evolution of the different generations of stars and the physical conditions of their surrounding gaseous nebulae through the photoionization of the gas, strong stellar winds, super-bubble formation and material flows. The analysis of these processes between a starburst and its environment requires the complete study of the gaseous component, from its kinematical structure to its physical properties. Using different observational techniques, low-inter mediate and high-spectral resolution spectroscopy, the physical conditions (electron density and temperatures), ionic and total chemical abundances of several atoms, reddening and ionization, structure, for the global flux and for the different kinematical components can be derive. Applying the direct method or empirical relationships for abundance determination, wc are able to perform a comparative analysis between different star-forming regions belonging to the same galaxy. The relative abundances of N/O, S/O, Ne/O and Ar/O for the different kinematical components give us clues for a common or very similar chemical evolution for the different kinematical components of each knot. It could also be indicative that the different kinematical components are different phases of the same gas. Similarities between the ionization structure of the different kinematical components could imply that the effective temperatures of the ionizing radiation fields are very similar for all the components, in spite of some small differences in the ionization state of different elements. The ionizing star clusters that excite the gas associated, to each star-forming knot that produces the different kinematical components could therefore be the same.Instituto de Astrofísica de La Plata2016-11info:eu-repo/semantics/conferenceObjectinfo:eu-repo/semantics/publishedVersionObjeto de conferenciahttp://purl.org/coar/resource_type/c_5794info:ar-repo/semantics/documentoDeConferenciaapplication/pdf39-48http://sedici.unlp.edu.ar/handle/10915/165640enginfo:eu-repo/semantics/altIdentifier/isbn/978-987-24948-5-8info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-10-22T17:24:55Zoai:sedici.unlp.edu.ar:10915/165640Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-10-22 17:24:56.103SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Chemodynamics of Star-Forming Regions
title Chemodynamics of Star-Forming Regions
spellingShingle Chemodynamics of Star-Forming Regions
Hägele, Guillermo Federico
Ciencias Astronómicas
star-forming regions
chemical evolution
title_short Chemodynamics of Star-Forming Regions
title_full Chemodynamics of Star-Forming Regions
title_fullStr Chemodynamics of Star-Forming Regions
title_full_unstemmed Chemodynamics of Star-Forming Regions
title_sort Chemodynamics of Star-Forming Regions
dc.creator.none.fl_str_mv Hägele, Guillermo Federico
Firpo, Verónica
Bosch, Guillermo Luis
Díaz, Ángeles I.
Morrell, Nidia Irene
Campuzano Castro, Federico
Cardaci, Mónica Viviana
author Hägele, Guillermo Federico
author_facet Hägele, Guillermo Federico
Firpo, Verónica
Bosch, Guillermo Luis
Díaz, Ángeles I.
Morrell, Nidia Irene
Campuzano Castro, Federico
Cardaci, Mónica Viviana
author_role author
author2 Firpo, Verónica
Bosch, Guillermo Luis
Díaz, Ángeles I.
Morrell, Nidia Irene
Campuzano Castro, Federico
Cardaci, Mónica Viviana
author2_role author
author
author
author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
star-forming regions
chemical evolution
topic Ciencias Astronómicas
star-forming regions
chemical evolution
dc.description.none.fl_txt_mv The large number of massive stars belonging to regions with violent star formation dominates the morphology of the gas, the evolution of the different generations of stars and the physical conditions of their surrounding gaseous nebulae through the photoionization of the gas, strong stellar winds, super-bubble formation and material flows. The analysis of these processes between a starburst and its environment requires the complete study of the gaseous component, from its kinematical structure to its physical properties. Using different observational techniques, low-inter mediate and high-spectral resolution spectroscopy, the physical conditions (electron density and temperatures), ionic and total chemical abundances of several atoms, reddening and ionization, structure, for the global flux and for the different kinematical components can be derive. Applying the direct method or empirical relationships for abundance determination, wc are able to perform a comparative analysis between different star-forming regions belonging to the same galaxy. The relative abundances of N/O, S/O, Ne/O and Ar/O for the different kinematical components give us clues for a common or very similar chemical evolution for the different kinematical components of each knot. It could also be indicative that the different kinematical components are different phases of the same gas. Similarities between the ionization structure of the different kinematical components could imply that the effective temperatures of the ionizing radiation fields are very similar for all the components, in spite of some small differences in the ionization state of different elements. The ionizing star clusters that excite the gas associated, to each star-forming knot that produces the different kinematical components could therefore be the same.
Instituto de Astrofísica de La Plata
description The large number of massive stars belonging to regions with violent star formation dominates the morphology of the gas, the evolution of the different generations of stars and the physical conditions of their surrounding gaseous nebulae through the photoionization of the gas, strong stellar winds, super-bubble formation and material flows. The analysis of these processes between a starburst and its environment requires the complete study of the gaseous component, from its kinematical structure to its physical properties. Using different observational techniques, low-inter mediate and high-spectral resolution spectroscopy, the physical conditions (electron density and temperatures), ionic and total chemical abundances of several atoms, reddening and ionization, structure, for the global flux and for the different kinematical components can be derive. Applying the direct method or empirical relationships for abundance determination, wc are able to perform a comparative analysis between different star-forming regions belonging to the same galaxy. The relative abundances of N/O, S/O, Ne/O and Ar/O for the different kinematical components give us clues for a common or very similar chemical evolution for the different kinematical components of each knot. It could also be indicative that the different kinematical components are different phases of the same gas. Similarities between the ionization structure of the different kinematical components could imply that the effective temperatures of the ionizing radiation fields are very similar for all the components, in spite of some small differences in the ionization state of different elements. The ionizing star clusters that excite the gas associated, to each star-forming knot that produces the different kinematical components could therefore be the same.
publishDate 2016
dc.date.none.fl_str_mv 2016-11
dc.type.none.fl_str_mv info:eu-repo/semantics/conferenceObject
info:eu-repo/semantics/publishedVersion
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dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/isbn/978-987-24948-5-8
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
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Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.format.none.fl_str_mv application/pdf
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