Abstract
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.
Highlights
Binary neutron star (BNS) mergers have been actively discussed as sources of multi-messenger astrophysics for a long time
We briefly review what we learned from GW170817, and discuss future prospects for high-energy neutrino detections and hadronic cosmic-ray production from neutron star mergers
We have briefly reviewed the multi-messenger event GW170817, future prospects for neutrino detections coincident with gravitational waves (GWs), and super-knee cosmic rays from the remnants of neutron star mergers
Summary
Binary neutron star (BNS) mergers have been actively discussed as sources of multi-messenger astrophysics for a long time. The protons are accelerated to very high energy there and interact with the target photons observed as SGRBs, producing pions that decay to the neutrinos. The multi-messenger observation of GW170817 confirmed most of the pictures above [18] This event was detected by the GWs, radio waves, optical, ultraviolet (UV), infrared (IR), X-rays, and MeV gamma-rays. GeV and TeV gamma-rays and neutrinos are not detected, despite that the BNS mergers are expected to emit these high-energy particles. The GW170817 observations give us the physical quantities of the macronova ejecta, which enables us to discuss the hadronic high-energy processes related to BNS mergers in more quantitative manner. We briefly review what we learned from GW170817, and discuss future prospects for high-energy neutrino detections and hadronic cosmic-ray production from neutron star mergers. The main topics of this paper (Section 3 and 4) are published in [19,20,21]
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