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Quasithermal neutrinos from rotating protoneutron stars born during core collapse of massive stars

Kohta Murase1,3, Basudeb Dasgupta2,3, and Todd A. Thompson3,4

  • 1Hubble Fellow—Institute for Advanced Study, Princeton, New Jersey 08540, USA
  • 2International Centre for Theoretical Physics, Trieste 34014, Italy
  • 3CCAPP, The Ohio State University, Columbus, Ohio 43210, USA
  • 4Department of Astronomy, The Ohio State University, Columbus, Ohio 43210, USA

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Phys. Rev. D 89, 043012 – Published 24 February, 2014

DOI: https://doi.org/10.1103/PhysRevD.89.043012

Abstract

Rotating and magnetized protoneutron stars may drive relativistic magnetocentrifugally accelerated winds as they cool immediately after core collapse. The wind fluid near the star is composed of neutrons and protons, and the neutrons become relativistic while collisionally coupled with the ions. Here, we argue that the neutrons in the flow eventually undergo inelastic collisions around the termination shock inside the stellar material, producing ∼0.1–1  GeV neutrinos, without relying on cosmic-ray acceleration mechanisms. Even higher-energy neutrinos may be produced via particle acceleration mechanisms. We show that Precision IceCube Next Generation Upgrade and Hyper-Kamiokande can detect such neutrinos from nearby core-collapse supernovae, by reducing the atmospheric neutrino background via coincident detection of MeV neutrinos or gravitational waves and optical observations. Detection of these GeV and/or higher-energy neutrinos would provide important clues to the physics of magnetic acceleration, nucleosynthesis, the relation between supernovae and gamma-ray bursts, and the properties of newly born neutron stars.

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See Also

Neutron-Proton-Converter Acceleration Mechanism at Subphotospheres of Relativistic Outflows

Kazumi Kashiyama, Kohta Murase, and Peter Mészáros
Phys. Rev. Lett. 111, 131103 (2013)

Article Text

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Phys. Rev. D 89, 043012– Published 24 February, 2014
  • Received 13 March 2013

© 2014 American Physical Society

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