Relatore
Ballelli, Matteo
(GSSI)
Descrizione
We present an improved parametric model for neutrino emission from core-collapse supernovae that directly connects neutrino luminosity and average energy to stellar properties during the emission. Our model incorporates two critical physical processes: convection within the proto-neutron star (PNS) and the evolving dynamics of neutrinosphere radii during the early emission phase. Crucially, the evolution of the PNS radius is tied to its gravitational-wave signature, providing a stronger physical framework for joint neutrino and gravitational-wave searches of the next Galactic supernova.
| Sessione | Onde Gravitazionali e astronomia multimessaggera |
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Autori
Ballelli, Matteo
(GSSI)
Prof.
Drago, Marco
(U. La Sapienza)
Pagliaroli, Giulia
(INFN- LNGS)
Dr.
Pompa, Federica
(Laboratori Nazionali del Gran Sasso - INFN)
Prof.
Ternes, Christoph
(GSSI)