- Inma Domínguez
- Univ. de Granada
- ICCUB - IEEC
- DAM seminar room (724), 7th floor
Thermonuclear explosions of carbon-oxygen white dwarfs (CO WDs), or Type Ia supernovae (SNIa) are important tools for cosmology. SNIa observations show the recent acceleration and previous deceleration of the expansion rate of the Universe, in agreement with a 70% of the energy-matter content of the Universe in form of dark energy. To constrain the nature of the dark energy, based on SNe Ia Hubble diagrams, it is necessary to decrease the current dispersion in the SNIa calibration relation. Observational data show that galaxies with on-going star formation host brighert SNIa. Models and observations agree that brighter SNIa require more 56Ni synthesized during the explosions. However, Why exploding CO WDs associated with young enviroments should produce more 56Ni ? This question challenges our understanding. In this talk, I will present numerical simulations that may allow to connect the SNIa calibration relation with progenitor metallicity.
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