Rotational Effects on Neutrino Emission in Core-collapse Supernovae

All stars rotate. While magnetic braking slows massive stars, the effect a stellar companion has on stellar rotation is still being explored. To prepare for future observations from rotating core-collapse supernovae (CCSNe), we analyze a set of 30 2D neutrino radiation-hydrodynamic CCSN simulations for a variety of compactness values, rotation rates, and equations of state. We systematically explore how rotation lowers expected neutrino counts and energies for a realistic detector, while accounting for adiabatic Mikheyev-Smirnov-Wolfenstein matter effects. We quantify the effect of viewing angle for neutrino emission for multiple rotation rates. Using ‘multimessenger synthesis’, we develop a technique that correlates multimessengers to constrain the neutrino mass ordering for a future supernova event. Likewise, we develop a method to constrain the distance to a rotating or nonrotating CCSN, regardless of explosion outcome.

💡 Research Summary

This paper presents a comprehensive investigation of how stellar rotation influences the neutrino emission from core‑collapse supernovae (CCSNe) and the observable signatures in realistic detectors. The authors performed 30 two‑dimensional (axisymmetric) neutrino radiation‑hydrodynamics simulations using the FLASH‑v4 framework with an energy‑dependent M1 transport scheme (12 energy bins up to 250 MeV) and a general‑relativistic effective potential (GREP) for gravity. The simulation suite combines 19 models from a previous study (Ref.