EPJ Web Conf.
Volume 210, 2019Ultra High Energy Cosmic Rays 2018 (UHECR 2018)
|Number of page(s)||9|
|Published online||17 May 2019|
High-energy emissions from neutron star mergers
Department of Physics, Pennsylvania State University, University Park, Pennsylvania, 16802, USA
2 Center for Particle and Gravitational Astrophysics, Pennsylvania State University, University Park, Pennsylvania, 16802, USA
3 Department of Astronomy & Astrophysics, Pennsylvania State University, University Park, Pennsylvania, 16802, USA
* e-mail: email@example.com
Published online: 17 May 2019
In 2017, LIGO-Virgo collaborations reported detection of the first neutron star merger event, GW170817, which is accompanied by electromagnetic counterparts from radio to gamma rays. Although high-energy neutrinos were not detected from this event, mergers of neutron stars are expected to produce such high-energy particles. Relativistic jets are launched when neutron stars merge. If the jets contain protons, they can emit high-energy neutrinos through photomeson production. In addition, neutron star mergers produce massive and fast ejecta, which can be a source of Galactic high-energy cosmic rays above the knee. We briefly review what we learned from the multi-messenger event, GW170817, and discuss prospects for multi-messenger detections and hadronic cosmic-ray production related to the neutron star mergers.
© The Authors, published by EDP Sciences, 2019
This is an open access article distributed under the terms of the Creative Commons Attribution License 4.0 (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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