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The hydrodynamic evolution of the gas content in the dSph galaxy Ursa Minor induced by the feedback from types Ia and II supernovae

Published online by Cambridge University Press:  30 October 2019

Anderson Caproni Open the ORCID record for Anderson Caproni [Opens in a new window] ,
Gustavo A. Lanfranchi ,
Gabriel H. Campos Baião ,
Grzegorz Kowal  and
Diego Falceta-Gonçalves
Anderson Caproni
Affiliation:
Núcleo de Astrofísica Teórica, Universidade Cruzeiro do Sul, R. Galvão Bueno 868, Liberdade, 01506-000, São Paulo, SP, Brazil email: anderson.caproni@cruzeirodosul.edu.br
Gustavo A. Lanfranchi
Affiliation:
Núcleo de Astrofísica Teórica, Universidade Cruzeiro do Sul, R. Galvão Bueno 868, Liberdade, 01506-000, São Paulo, SP, Brazil email: anderson.caproni@cruzeirodosul.edu.br
Gabriel H. Campos Baião
Affiliation:
Núcleo de Astrofísica Teórica, Universidade Cruzeiro do Sul, R. Galvão Bueno 868, Liberdade, 01506-000, São Paulo, SP, Brazil email: anderson.caproni@cruzeirodosul.edu.br
Grzegorz Kowal
Affiliation:
Escola de Artes, Ciências e Humanidades, Universidade de São Paulo, Rua Arlindo Bettio 1000, CEP 03828-000 São Paulo, Brazil
Diego Falceta-Gonçalves
Affiliation:
Escola de Artes, Ciências e Humanidades, Universidade de São Paulo, Rua Arlindo Bettio 1000, CEP 03828-000 São Paulo, Brazil
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Abstract

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Dwarf spheroidal galaxies of the Local Group share a similar characteristic nowadays: a low amount of gas in their interiors. In this work, we present results from a three-dimensional hydrodynamical simulation of the gas inside an object with similar characteristics of the Ursa Minor galaxy. We evolved the initial gas distribution over 3 Gyr, considering the effects of the types Ia and II supernovae. The instantaneous supernovae rates were derived from a chemical evolution model applied to spectroscopic data of the Ursa Minor galaxy. Our simulation shows that the amount of gas that is lost varies with time and galactocentric radius. The highest gas-loss rates occurred during the first 600 Myr of evolution. Our results also indicate that types Ia and II supernovae must be essential drivers of the gas loss in Ursa Minor galaxy (and probably in other similar dwarf galaxies).

Keywords

galaxies: dwarfgalaxies: evolutiongalaxies: individual (Ursa Minor)galaxies: ISMhydrodynamicsmethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S344: Dwarf Galaxies: From the Deep Universe to the Present , August 2018 , pp. 49 - 52
Copyright
© International Astronomical Union 2019 

References

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