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000407652 1001_ $$0P:(DE-H253)PIP1003168$$aLindner, Axel$$b0$$eEditor
000407652 1112_ $$0C18-06-18.7$$2inspire$$a14th "Patras" Workshop on Axions, WIMPs and WISPs$$cHamburg$$d2018-06-18 - 2018-06-22$$gPATRAS 2018$$wGermany
000407652 245__ $$aAxions, WIMPs and WISPs$$bproceedings, 14th Patras workshop, PATRAS 2018, Hamburg, Germany, June 18-22, 2018$$cEditors: Axel Lindner, Todd Kozlowski
000407652 260__ $$aHamburg$$bVerlag Deutsches Elektronen-Synchrotron$$c2018
000407652 300__ $$aviii, 103 pages : illustrations
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000407652 520__ $$aA Galactic supernova (SN) axion signal would be detected in a future neutrino Mton-class water Cherenkov detector, such as the proposed Hyper-Kamiokande in Japan. The main detection channel for axions is absorption on the oxygen nuclei in the water. The subsequent oxygen de-excitation leads to a potentially detectable gamma signal. In this contribution we present a calculation of the SN axion signal and discuss its detectability in Hyper-Kamiokande.
000407652 536__ $$0G:(DE-HGF)POF3-6211$$a6211 - Extreme States of Matter: From Cold Ions to Hot Plasmas (POF3-621)$$cPOF3-621$$fPOF III$$x0
000407652 650_7 $$2DE-H253$$aWeakly interacting slim particle
000407652 650_7 $$2DE-H253$$aWeakly interacting slender particle
000407652 650_7 $$2DE-H253$$aWeakly interacting sub-eV particle
000407652 650_7 $$2DE-H253$$aPATRAS 2018
000407652 650_7 $$2DE-H253$$aWIMPs
000407652 650_7 $$2DE-H253$$aAxions
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000407652 650_7 $$2DE-H253$$aWeakly interacting massive particles
000407652 650_7 $$2DE-H253$$aHamburg
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000407652 7001_ $$0P:(DE-H253)PIP1080659$$aKozlowski, Todd$$b1$$eEditor
000407652 7870_ $$0PUBDB-2021-00114$$aCarenza, Pierluca et.al.$$d2019$$iIsMemberOf$$rarXiv:1808.04101 ; DESY-PROC-2018-03$$tAxion emission and detection from a Galactic supernova
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