Supernova Model Discrimination with Hyper-Kamiokande. (arXiv:2101.05269v2 [astro-ph.IM] UPDATED)

Supernova Model Discrimination with Hyper-Kamiokande. (arXiv:2101.05269v2 [astro-ph.IM] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_Hyper_Kamiokande/0/1/0/all/0/1">Hyper-Kamiokande Collaboration</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Abe_K/0/1/0/all/0/1">K. Abe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adrich_P/0/1/0/all/0/1">P. Adrich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aihara_H/0/1/0/all/0/1">H. Aihara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Akutsu_R/0/1/0/all/0/1">R. Akutsu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alekseev_I/0/1/0/all/0/1">I. Alekseev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ali_A/0/1/0/all/0/1">A. Ali</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ameli_F/0/1/0/all/0/1">F. Ameli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anghel_I/0/1/0/all/0/1">I. Anghel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anthony_L/0/1/0/all/0/1">L.H.V. Anthony</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Antonova_M/0/1/0/all/0/1">M. Antonova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Araya_A/0/1/0/all/0/1">A. Araya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asaoka_Y/0/1/0/all/0/1">Y. Asaoka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ashida_Y/0/1/0/all/0/1">Y. Ashida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aushev_V/0/1/0/all/0/1">V. Aushev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ballester_F/0/1/0/all/0/1">F. Ballester</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bandac_I/0/1/0/all/0/1">I. Bandac</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barbi_M/0/1/0/all/0/1">M. Barbi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barker_G/0/1/0/all/0/1">G.J. Barker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barr_G/0/1/0/all/0/1">G. Barr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Batkiewicz_Kwasniak_M/0/1/0/all/0/1">M. Batkiewicz-Kwasniak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bellato_M/0/1/0/all/0/1">M. Bellato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berardi_V/0/1/0/all/0/1">V. Berardi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bergevin_M/0/1/0/all/0/1">M. Bergevin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernard_L/0/1/0/all/0/1">L. Bernard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernardini_E/0/1/0/all/0/1">E. Bernardini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berns_L/0/1/0/all/0/1">L. Berns</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhadra_S/0/1/0/all/0/1">S. Bhadra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bian_J/0/1/0/all/0/1">J. Bian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blanchet_A/0/1/0/all/0/1">A. Blanchet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blaszczyk_F/0/1/0/all/0/1">F.d.M. Blaszczyk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blondel_A/0/1/0/all/0/1">A. Blondel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boiano_A/0/1/0/all/0/1">A. Boiano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bolognesi_S/0/1/0/all/0/1">S. Bolognesi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonavera_L/0/1/0/all/0/1">L. Bonavera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Booth_N/0/1/0/all/0/1">N. Booth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Borjabad_S/0/1/0/all/0/1">S. Borjabad</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boschi_T/0/1/0/all/0/1">T. Boschi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bose_D/0/1/0/all/0/1">D. Bose</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boyd_S/0/1/0/all/0/1">S .B. Boyd</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bozza_C/0/1/0/all/0/1">C. Bozza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bravar_A/0/1/0/all/0/1">A. Bravar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bravo_Berguno_D/0/1/0/all/0/1">D. Bravo-Berguño</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bronner_C/0/1/0/all/0/1">C. Bronner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brown_L/0/1/0/all/0/1">L. Brown</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bubak_A/0/1/0/all/0/1">A. Bubak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buchowicz_A/0/1/0/all/0/1">A. Buchowicz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avanzini_M/0/1/0/all/0/1">M. Buizza Avanzini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cafagna_F/0/1/0/all/0/1">F. S. Cafagna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calabria_N/0/1/0/all/0/1">N. F. Calabria</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calvo_Mozota_J/0/1/0/all/0/1">J. M. Calvo-Mozota</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cao_S/0/1/0/all/0/1">S. Cao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cartwright_S/0/1/0/all/0/1">S.L. Cartwright</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carroll_A/0/1/0/all/0/1">A. Carroll</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Catanesi_M/0/1/0/all/0/1">M. G. Catanesi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cebrian_S/0/1/0/all/0/1">S. Cebriàn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chabera_M/0/1/0/all/0/1">M. Chabera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chakraborty_S/0/1/0/all/0/1">S. Chakraborty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Checchia_C/0/1/0/all/0/1">C. Checchia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choi_J/0/1/0/all/0/1">J. H. Choi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choubey_S/0/1/0/all/0/1">S. Choubey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cicerchia_M/0/1/0/all/0/1">M. Cicerchia</a>, et al. (440 additional authors not shown)

Core-collapse supernovae are among the most magnificent events in the
observable universe. They produce many of the chemical elements necessary for
life to exist and their remnants — neutron stars and black holes — are
interesting astrophysical objects in their own right. However, despite
millennia of observations and almost a century of astrophysical study, the
explosion mechanism of core-collapse supernovae is not yet well understood.
Hyper-Kamiokande is a next-generation neutrino detector that will be able to
observe the neutrino flux from the next galactic core-collapse supernova in
unprecedented detail. We focus on the first 500 ms of the neutrino burst,
corresponding to the accretion phase, and use a newly-developed, high-precision
supernova event generator to simulate Hyper-Kamiokande’s response to five
different supernova models. We show that Hyper-Kamiokande will be able to
distinguish between these models with high accuracy for a supernova at a
distance of up to 100 kpc. Once the next galactic supernova happens, this
ability will be a powerful tool for guiding simulations towards a precise
reproduction of the explosion mechanism observed in nature.

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