Busca avançada
Ano de início
Entree
(Referência obtida automaticamente do Web of Science, por meio da informação sobre o financiamento pela FAPESP e o número do processo correspondente, incluída na publicação pelos autores.)

THREE-DIMENSIONAL HYDRODYNAMICAL SIMULATIONS OF THE SUPERNOVAE-DRIVEN GAS LOSS IN THE DWARF SPHEROIDAL GALAXY URSA MINOR

Texto completo
Autor(es):
Caproni, A. [1] ; Lanfranchi, G. A. [1] ; Luiz da Silva, A. [1, 2] ; Falceta-Goncalves, D. [3, 4]
Número total de Autores: 4
Afiliação do(s) autor(es):
[1] Univ Cruzeiro Sul, Nucl Astrofis Teor, BR-01506000 Sao Paulo - Brazil
[2] Univ Sao Paulo, Observ Dietrich Schiel, Ctr Divulgacao Astron, Sao Carlos, SP - Brazil
[3] Univ Sao Paulo, Escola Artes Ciencias & Humanidades, BR-03828000 Sao Paulo - Brazil
[4] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife - Scotland
Número total de Afiliações: 4
Tipo de documento: Artigo Científico
Fonte: ASTROPHYSICAL JOURNAL; v. 805, n. 2 JUN 1 2015.
Citações Web of Science: 4
Resumo

As is usual in dwarf spheroidal galaxies, today the Local Group galaxy Ursa Minor is depleted of its gas content. How this galaxy lost its gas is still a matter of debate. To study the history of gas loss in Ursa Minor, we conducted the first three-dimensional hydrodynamical simulations of this object, assuming that the gas loss was driven by galactic winds powered only by type II supernovae (SNe II). The initial gas setup and supernova (SN) rates used in our simulations are mainly constrained by the inferred star formation history and the observed velocity dispersion of Ursa Minor. After 3 Gyr of evolution, we found that the gas removal efficiency is higher when the SN rate is increased, and also when the initial mean gas density is lowered. The derived mass-loss rates are systematically higher in the central regions (<300 pc), even though such a relationship has not been strictly linear in time and in terms of the galactic radius. The filamentary structures induced by Rayleigh-Taylor instabilities and the concentric shells related to the acoustic waves driven by SNe can account for the inferred mass losses from the simulations. Our results suggest that SNe II are able to transfer most of the gas from the central region outward to the galactic halo. However, other physical mechanisms must be considered in order to completely remove the gas at larger radii. (AU)

Processo FAPESP: 15/06361-0 - Three-dimensional hydrodynamical simulations of the supernovae-driven gas loss in the Dwarf Spheroidal Galaxy Ursa minor
Beneficiário:Anderson Caproni
Linha de fomento: Auxílio à Pesquisa - Publicações científicas - Artigo
Processo FAPESP: 11/12909-8 - Campos magnéticos, turbulência e efeitos de plasma no meio intergaláctico
Beneficiário:Diego Antonio Falceta Gonçalves
Linha de fomento: Auxílio à Pesquisa - Regular
Processo FAPESP: 09/54006-4 - Um cluster de computadores para o Departamento de Astronomia do IAG-USP e para o Núcleo de Astrofísica da UNICSUL
Beneficiário:Elisabete Maria de Gouveia Dal Pino
Linha de fomento: Auxílio à Pesquisa - Programa Equipamentos Multiusuários