Why galaxies care about Type Ia Supernovae?

Noelia Jiménez, Patricia B. Tissera, Francesca Matteucci

Resultado de la investigación: Article

Resumen

We implement the Single Degenerate (SD) scenario proposed for Type Ia Supernova (SNIa) progenitors in SPH simulations. We analyse the chemical evolution of bulge-type galaxies together with the observed correlations relating SNIa rates with the characteristics of the host galaxy, such as their SFR. The models reproduce the observed signatures shown by [O/Fe] ratios in the Galactic Bulge and the present day SNIa rates. Also, the observed correlation found by Sullivan et al. (2006) between SSFR (specific star formation rate) and the SNIa rate per unit of galaxy mass (SSNIaR), naturally arises. This analysis helps to set more stringent constraints to the galaxy formation models and gives some hint on the progenitor problem.

Idioma originalEnglish
Páginas (desde-hasta)206-209
Número de páginas4
PublicaciónProceedings of the International Astronomical Union
Volumen10
DOI
EstadoPublished - 2014

Huella dactilar

supernovae
galaxies
galactic bulge
chemical evolution
galactic evolution
star formation rate
signatures
rate
simulation

ASJC Scopus subject areas

  • Astronomy and Astrophysics

Citar esto

Jiménez, Noelia ; Tissera, Patricia B. ; Matteucci, Francesca. / Why galaxies care about Type Ia Supernovae?. En: Proceedings of the International Astronomical Union. 2014 ; Vol. 10. pp. 206-209.
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Why galaxies care about Type Ia Supernovae? / Jiménez, Noelia; Tissera, Patricia B.; Matteucci, Francesca.

En: Proceedings of the International Astronomical Union, Vol. 10, 2014, p. 206-209.

Resultado de la investigación: Article

TY - JOUR

T1 - Why galaxies care about Type Ia Supernovae?

AU - Jiménez, Noelia

AU - Tissera, Patricia B.

AU - Matteucci, Francesca

PY - 2014

Y1 - 2014

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AB - We implement the Single Degenerate (SD) scenario proposed for Type Ia Supernova (SNIa) progenitors in SPH simulations. We analyse the chemical evolution of bulge-type galaxies together with the observed correlations relating SNIa rates with the characteristics of the host galaxy, such as their SFR. The models reproduce the observed signatures shown by [O/Fe] ratios in the Galactic Bulge and the present day SNIa rates. Also, the observed correlation found by Sullivan et al. (2006) between SSFR (specific star formation rate) and the SNIa rate per unit of galaxy mass (SSNIaR), naturally arises. This analysis helps to set more stringent constraints to the galaxy formation models and gives some hint on the progenitor problem.

KW - Galaxies: evolution

KW - Galaxies: formation

KW - Galaxies: numerical simulations

KW - Galaxies: supernovae

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