Diagnosing the Structure of Massive Stars with Galactic Supernova Neutrinos

2018/04/30 by Shunsaku Horiuchi, Ko Nakamura, Horiuchi, Shunsaku +5
Physics and Astronomy · #FOS: Physical sciences #High Energy Astrophysical Phenomena (astro-ph.HE) #astro-ph.HE

paper · pdf · doi:10.48550/arxiv.1805.00050

Poster presented at NuPhys2017 (London, 20-22 December 2017). 5 pages, LaTeX, 3 figures

arxiv created 2018/04/30 · arxiv updated 2018/05/02

Abstract

It has been suggested that whether a star explodes or not, and what kind of explosion properties it shows, is strongly dependent on the progenitor's core structure. We present the results from 101 axisymmetric core-collapse supernova simulations performed with progenitors spanning initial masses in the range from 10.8 to 75 solar masses, and focus on their connections to the compactness of the progenitor's core. Our simulations confirm a correlation between the neutrinos emitted during the accretion phase and the progenitor's compactness. We suggest that the ratio of observed neutrino events during the first hundreds of milliseconds can be used to infer the progenitor's inner mass density structure.

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