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The gas-loss evolution in dwarf spheroidal galaxies: Supernova feedback and environment effects in the case of the local group galaxy Ursa Minor

Published online by Cambridge University Press:  29 March 2021

Anderson Caproni Open the ORCID record for Anderson Caproni [Opens in a new window]  and
Gustavo Amaral Lanfranchi Open the ORCID record for Gustavo Amaral Lanfranchi [Opens in a new window]
Anderson Caproni
Affiliation:
Núcleo de Astrofísica, Universidade Cidade de São Paulo, R. Galvão Bueno 868, Liberdade, São Paulo, SP, 01506-000, Brazil email: anderson.caproni@cruzeirodosul.edu.br
Gustavo Amaral Lanfranchi
Affiliation:
Núcleo de Astrofísica, Universidade Cidade de São Paulo, R. Galvão Bueno 868, Liberdade, São Paulo, SP, 01506-000, Brazil email: anderson.caproni@cruzeirodosul.edu.br
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Abstract

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In this work, we performed two distinct non-cosmological, three-dimensional hydrodynamic simulations that evolved the gas component of a galaxy similar to the classical dwarf spheroidal galaxy Ursa Minor. Both simulations take into account types II and Ia supernovae feedback constrained by chemical evolution models, while ram-pressure stripping mechanism is added into one of them considering an intergalactic medium and a galactic velocity that resemble what is observed nowadays for the Ursa Minor galaxy. Our results show no difference in the amount of gas left inside the galaxy until 400 Myr of evolution. Moreover, the ram-pressure wind was stalled and inverted by thermal pressure of the interstellar medium and supernovae feedback during the same interval.

Keywords

galaxies: dwarfgalaxies: evolutiongalaxies: individual(Ursa Minor)galaxies: ISMhydrodynamicsmethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S359: Galaxy Evolution and Feedback across Different Environments , March 2019 , pp. 117 - 118
Copyright
© The Author(s), 2021. Published by Cambridge University Press on behalf of International Astronomical Union

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