Speaker
Description
The gravitational radiation from core-collapse supernovae (CCSNe) is dominated by the oscillation modes of the proto-neutron star associated and the stalled accretion shock, and can be detectable in the case of galactic distances. These modes have been computed by several methods [1, 2, 3]. In this talk, we present the first steps of a potential alternative method to classify the different eigenmodes, based on linear similarity among the different modes, as well as other techniques, starting from some simplified cases and taking into account more realistic CCSNe scenarios. This work aims at providing information for asteroseismology of CCSNe from gravitational-wave future observations data. [1] MNRAS 474, 5272--5286 (2018). [2] MNRAS 482, 3967--3988 (2019). [3] arXiv:2504.12183 (2025).
