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Published January 10, 2013 | Published + Submitted
Journal Article Open

The Progenitor Dependence of the Preexplosion Neutrino Emission in Core-Collapse Supernovae


We perform spherically symmetric general-relativistic simulations of core collapse and the postbounce pre-explosion phase in 32 presupernova stellar models of solar metallicity with zero-age main-sequence masses of 12-120 M_☉. Using energy-dependent three-species neutrino transport in the two-moment approximation with an analytic closure, we show that the emitted neutrino luminosities and spectra follow very systematic trends that are correlated with the compactness (~M/R) of the progenitor star's inner regions via the accretion rate in the pre-explosion phase. We find that these qualitative trends depend only weakly on the nuclear equation of state (EOS), but quantitative observational statements will require independent constraints on the EOS and the rotation rate of the core as well as a more complete understanding of neutrino oscillations. We investigate the simulated response of water Cherenkov detectors to the electron antineutrino fluxes from our models and find that the large statistics of a galactic core collapse event may allow robust conclusions on the inner structure of the progenitor star.

Additional Information

© 2013 American Astronomical Society. Received 2012 July 4; accepted 2012 November 16; published 2012 December 21. We acknowledge helpful discussions with and input from John Beacom, Adam Burrows, Luc Dessart, Ken Nomoto, Ryan Patterson, Kate Scholberg, Mark Vagins, and Stan Woosley. C.D.O. thanks the Kavli Institute for the Physics and Mathematics of the Universe for hospitality while work on a draft of this article was carried out. The computations were performed at Caltech's Center for Advanced Computing Research on the cluster "Zwicky" funded through NSF grant No. PHY-0960291 and the Sherman Fairchild Foundation. Furthermore, computations were performed on Louisiana Optical Network Infrastructure computer systems under allocation loni_numrel06, on the NSF XSEDE Network under allocation TG-PHY100033, and on resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. EOC is supported in part by a postgraduate fellowship from the Natural Sciences and Engineering Research Council of Canada (NSERC). This research is supported in part by the National Science Foundation under grant Nos. AST-0855535 and OCI-0905046, by the Alfred P. Sloan Foundation, and by the Sherman Fairchild Foundation.

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Published - 0004-637X_762_2_126.pdf

Submitted - 1207.1100v1.pdf


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