Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies
- Autores
- Nuza, Sebastian Ernesto; Scannapieco, Cecilia; Chiappini, Cristina; Junqueira, Thiago C.; Minchev, Ivan; Martig, Marie
- Año de publicación
- 2019
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- One of the fundamental assumptions of chemical evolution models (CEMs) of the Milky Way (MW) and other spirals is that higher gas accretion rates are expected in the past, and in the inner regions of the Galaxy. This leads to the so-called 'inside-out disc formation scenario'. Yet, these are probably the most unconstrained inputs of such models. In this paper, we aim at investigating these main assumptions by studying how gas is accreted in four simulated MW-like galaxies assembled within the ΛCDM scenario. The galaxies were obtained using two different simulation techniques, cosmological setups, and initial conditions. Two of them are MW candidates corresponding to the chemodynamical model of Minchev, Chiappini & Martig (known as MCM) and the Local Group cosmological simulation of Nuza et al. We investigate vertical and radial gas accretion on to galaxy discs as a function of cosmic time and disc radius. We find that accretion in the MW-like galaxies seem to happen in two distinct phases, namely, an early, more violent period; followed by a subsequent, slowly declining phase. Our simulations seem to give support to the assumption that the amount of gas incorporated into the MW disc exponentially decreases with time, leading to current net accretion rates of 0.6-1 M⊙ yr-1. In particular, accretion time-scales on to the simulated thin-disc-like structures are within ∼5-7 Gyr, consistent with expectations from CEMs. Moreover, our simulated MW discs are assembled from the inside-out with gas in the inner disc regions accreted in shorter time-scales than in external ones, in qualitative agreement with CEMs of the Galaxy. However, this type of growth is not general to all galaxies and it is intimately linked to their particular merger and gas accretion history.
Fil: Nuza, Sebastian Ernesto. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina. Leibniz-Institut für Astrophysik Potsdam; Alemania
Fil: Scannapieco, Cecilia. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Departamento de Física; Argentina. Leibniz-Institut für Astrophysik Potsdam; Alemania. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Houssay; Argentina
Fil: Chiappini, Cristina. Leibniz Institut Fuer Astrophysik Potsdam; Alemania
Fil: Junqueira, Thiago C.. Leibniz Institut Fuer Astrophysik Potsdam; Alemania
Fil: Minchev, Ivan. Leibniz Institut Fuer Astrophysik Potsdam; Alemania
Fil: Martig, Marie. Liverpool John Moores University; Reino Unido - Materia
-
GALAXIES: EVOLUTION
GALAXIES: FORMATION
HYDRODYNAMICS
INTERGALACTIC MEDIUM
METHODS: NUMERICAL - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/113150
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Gas accretion in Milky Way-like galaxies: Temporal and radial dependenciesNuza, Sebastian ErnestoScannapieco, CeciliaChiappini, CristinaJunqueira, Thiago C.Minchev, IvanMartig, MarieGALAXIES: EVOLUTIONGALAXIES: FORMATIONHYDRODYNAMICSINTERGALACTIC MEDIUMMETHODS: NUMERICALhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1One of the fundamental assumptions of chemical evolution models (CEMs) of the Milky Way (MW) and other spirals is that higher gas accretion rates are expected in the past, and in the inner regions of the Galaxy. This leads to the so-called 'inside-out disc formation scenario'. Yet, these are probably the most unconstrained inputs of such models. In this paper, we aim at investigating these main assumptions by studying how gas is accreted in four simulated MW-like galaxies assembled within the ΛCDM scenario. The galaxies were obtained using two different simulation techniques, cosmological setups, and initial conditions. Two of them are MW candidates corresponding to the chemodynamical model of Minchev, Chiappini & Martig (known as MCM) and the Local Group cosmological simulation of Nuza et al. We investigate vertical and radial gas accretion on to galaxy discs as a function of cosmic time and disc radius. We find that accretion in the MW-like galaxies seem to happen in two distinct phases, namely, an early, more violent period; followed by a subsequent, slowly declining phase. Our simulations seem to give support to the assumption that the amount of gas incorporated into the MW disc exponentially decreases with time, leading to current net accretion rates of 0.6-1 M⊙ yr-1. In particular, accretion time-scales on to the simulated thin-disc-like structures are within ∼5-7 Gyr, consistent with expectations from CEMs. Moreover, our simulated MW discs are assembled from the inside-out with gas in the inner disc regions accreted in shorter time-scales than in external ones, in qualitative agreement with CEMs of the Galaxy. However, this type of growth is not general to all galaxies and it is intimately linked to their particular merger and gas accretion history.Fil: Nuza, Sebastian Ernesto. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina. Leibniz-Institut für Astrophysik Potsdam; AlemaniaFil: Scannapieco, Cecilia. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Departamento de Física; Argentina. Leibniz-Institut für Astrophysik Potsdam; Alemania. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Houssay; ArgentinaFil: Chiappini, Cristina. Leibniz Institut Fuer Astrophysik Potsdam; AlemaniaFil: Junqueira, Thiago C.. Leibniz Institut Fuer Astrophysik Potsdam; AlemaniaFil: Minchev, Ivan. Leibniz Institut Fuer Astrophysik Potsdam; AlemaniaFil: Martig, Marie. Liverpool John Moores University; Reino UnidoWiley Blackwell Publishing, Inc2019-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/113150Nuza, Sebastian Ernesto; Scannapieco, Cecilia; Chiappini, Cristina; Junqueira, Thiago C.; Minchev, Ivan; et al.; Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 482; 3; 1-2019; 3089-31080035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/sty2882info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/482/3/3089/5144234info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:51:47Zoai:ri.conicet.gov.ar:11336/113150instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 09:51:48.122CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies |
title |
Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies |
spellingShingle |
Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies Nuza, Sebastian Ernesto GALAXIES: EVOLUTION GALAXIES: FORMATION HYDRODYNAMICS INTERGALACTIC MEDIUM METHODS: NUMERICAL |
title_short |
Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies |
title_full |
Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies |
title_fullStr |
Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies |
title_full_unstemmed |
Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies |
title_sort |
Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies |
dc.creator.none.fl_str_mv |
Nuza, Sebastian Ernesto Scannapieco, Cecilia Chiappini, Cristina Junqueira, Thiago C. Minchev, Ivan Martig, Marie |
author |
Nuza, Sebastian Ernesto |
author_facet |
Nuza, Sebastian Ernesto Scannapieco, Cecilia Chiappini, Cristina Junqueira, Thiago C. Minchev, Ivan Martig, Marie |
author_role |
author |
author2 |
Scannapieco, Cecilia Chiappini, Cristina Junqueira, Thiago C. Minchev, Ivan Martig, Marie |
author2_role |
author author author author author |
dc.subject.none.fl_str_mv |
GALAXIES: EVOLUTION GALAXIES: FORMATION HYDRODYNAMICS INTERGALACTIC MEDIUM METHODS: NUMERICAL |
topic |
GALAXIES: EVOLUTION GALAXIES: FORMATION HYDRODYNAMICS INTERGALACTIC MEDIUM METHODS: NUMERICAL |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
One of the fundamental assumptions of chemical evolution models (CEMs) of the Milky Way (MW) and other spirals is that higher gas accretion rates are expected in the past, and in the inner regions of the Galaxy. This leads to the so-called 'inside-out disc formation scenario'. Yet, these are probably the most unconstrained inputs of such models. In this paper, we aim at investigating these main assumptions by studying how gas is accreted in four simulated MW-like galaxies assembled within the ΛCDM scenario. The galaxies were obtained using two different simulation techniques, cosmological setups, and initial conditions. Two of them are MW candidates corresponding to the chemodynamical model of Minchev, Chiappini & Martig (known as MCM) and the Local Group cosmological simulation of Nuza et al. We investigate vertical and radial gas accretion on to galaxy discs as a function of cosmic time and disc radius. We find that accretion in the MW-like galaxies seem to happen in two distinct phases, namely, an early, more violent period; followed by a subsequent, slowly declining phase. Our simulations seem to give support to the assumption that the amount of gas incorporated into the MW disc exponentially decreases with time, leading to current net accretion rates of 0.6-1 M⊙ yr-1. In particular, accretion time-scales on to the simulated thin-disc-like structures are within ∼5-7 Gyr, consistent with expectations from CEMs. Moreover, our simulated MW discs are assembled from the inside-out with gas in the inner disc regions accreted in shorter time-scales than in external ones, in qualitative agreement with CEMs of the Galaxy. However, this type of growth is not general to all galaxies and it is intimately linked to their particular merger and gas accretion history. Fil: Nuza, Sebastian Ernesto. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina. Leibniz-Institut für Astrophysik Potsdam; Alemania Fil: Scannapieco, Cecilia. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Departamento de Física; Argentina. Leibniz-Institut für Astrophysik Potsdam; Alemania. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Houssay; Argentina Fil: Chiappini, Cristina. Leibniz Institut Fuer Astrophysik Potsdam; Alemania Fil: Junqueira, Thiago C.. Leibniz Institut Fuer Astrophysik Potsdam; Alemania Fil: Minchev, Ivan. Leibniz Institut Fuer Astrophysik Potsdam; Alemania Fil: Martig, Marie. Liverpool John Moores University; Reino Unido |
description |
One of the fundamental assumptions of chemical evolution models (CEMs) of the Milky Way (MW) and other spirals is that higher gas accretion rates are expected in the past, and in the inner regions of the Galaxy. This leads to the so-called 'inside-out disc formation scenario'. Yet, these are probably the most unconstrained inputs of such models. In this paper, we aim at investigating these main assumptions by studying how gas is accreted in four simulated MW-like galaxies assembled within the ΛCDM scenario. The galaxies were obtained using two different simulation techniques, cosmological setups, and initial conditions. Two of them are MW candidates corresponding to the chemodynamical model of Minchev, Chiappini & Martig (known as MCM) and the Local Group cosmological simulation of Nuza et al. We investigate vertical and radial gas accretion on to galaxy discs as a function of cosmic time and disc radius. We find that accretion in the MW-like galaxies seem to happen in two distinct phases, namely, an early, more violent period; followed by a subsequent, slowly declining phase. Our simulations seem to give support to the assumption that the amount of gas incorporated into the MW disc exponentially decreases with time, leading to current net accretion rates of 0.6-1 M⊙ yr-1. In particular, accretion time-scales on to the simulated thin-disc-like structures are within ∼5-7 Gyr, consistent with expectations from CEMs. Moreover, our simulated MW discs are assembled from the inside-out with gas in the inner disc regions accreted in shorter time-scales than in external ones, in qualitative agreement with CEMs of the Galaxy. However, this type of growth is not general to all galaxies and it is intimately linked to their particular merger and gas accretion history. |
publishDate |
2019 |
dc.date.none.fl_str_mv |
2019-01 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
format |
article |
status_str |
publishedVersion |
dc.identifier.none.fl_str_mv |
http://hdl.handle.net/11336/113150 Nuza, Sebastian Ernesto; Scannapieco, Cecilia; Chiappini, Cristina; Junqueira, Thiago C.; Minchev, Ivan; et al.; Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 482; 3; 1-2019; 3089-3108 0035-8711 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/113150 |
identifier_str_mv |
Nuza, Sebastian Ernesto; Scannapieco, Cecilia; Chiappini, Cristina; Junqueira, Thiago C.; Minchev, Ivan; et al.; Gas accretion in Milky Way-like galaxies: Temporal and radial dependencies; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 482; 3; 1-2019; 3089-3108 0035-8711 CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/sty2882 info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/482/3/3089/5144234 |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
dc.format.none.fl_str_mv |
application/pdf application/pdf |
dc.publisher.none.fl_str_mv |
Wiley Blackwell Publishing, Inc |
publisher.none.fl_str_mv |
Wiley Blackwell Publishing, Inc |
dc.source.none.fl_str_mv |
reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) |
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CONICET Digital (CONICET) |
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Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
repository.mail.fl_str_mv |
dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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13.070432 |