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Résumé |
Accurately modeling neutrino flavor oscillations in global simulations of core-
collapse supernovae or neutron star mergers remains a major challenge, albeit a
potentially crucial one for making reliable predictions. Indeed, it is now widely
recognized that flavor instabilities—in which classically computed neutrino
distributions are dramatically altered when including quantum effects—must occur
commonly in such environments.
In this talk, I will focus on the case of binary neutron star mergers, and
specifically discuss so-called "fast" and "collisional" instabilities, trying to
answer a few questions. Where and when do they occur? What are their consequences?
To address the latter point, a promising strategy is the development of subgrid
models of neutrino flavor transformation. In this approach, insights from detailed
studies of local quantum neutrino transport are used to formulate effective
prescriptions that modify classical neutrino distributions, enabling their
incorporation into large-scale simulations. I will thus discuss recent progress on
determining the asymptotic states reached after the onset of a flavor instability,
a key ingredient for such subgrid models. |
