High-energy Neutrino Emission from Short Gamma-Ray Bursts: Prospects for Coincident Detection with Gravitational Waves

2019

Phys. Rev. D

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Transrelativistic supernovae (SNe), which are likely driven by central engines via jets or winds, have been among candidate sources of ultrahigh-energy cosmic rays (UHECRs). We investigate acceleration and survival of UHECR nuclei in the external reverse shock scenario. With composition models used in Zhang et al. (2018), we calculate spectra of escaping cosmic rays and secondary neutrinos. If their local rate is ∼ 1% of the core-collapse supernova rate, the observed UHECR spectrum and composition can be explained with the total cosmic-ray energy Ecr ∼ 10 51 erg. The maximum energy of UHECR nuclei can reach ∼ 10 20 − 10 21 eV. The diffuse flux of source neutrinos is predicted to be ∼ 10 −11 − 10 −10 GeV cm −2 s −1 sr −1 in the 0.1-1 EeV range, satisfying nucleussurvival bounds. The associated cosmogenic neutrino flux is calculated, and shown to be comparable or even higher than the source neutrino flux. These ultrahigh-energy neutrinos can be detected by ultimate detectors such as the Giant Radio Askaryan Neutrino Detector and Probe Of Extreme Multi-Messenger Astrophysics.

Section: 116]mentioning

confidence: 99%

Ultrahigh-energy cosmic-ray nuclei and neutrinos from engine-driven supernovae

Zhang

2019

Phys. Rev. D

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“…Whereas SGRBs are mainly detected as short hard bursts with a duration of ∼ < 2 s (e.g., Piran 2004;Nakar 2007;Gehrels et al 2009;Berger 2014;Ackermann et al 2013), it is known that a good fraction of SGRBs have late-time emission such as extended softer emission, X-ray flares, and plateaus (Evans et al 2009;Chincarini et al 2010;Margutti et al 2011;Sakamoto et al 2011;Rowlinson et al 2013;Kagawa et al 2015;Kaneko et al 2015;Lien et al 2016;Kisaka et al 2017), and even longer mysterious X-ray excess emission was reported for GRB 130603B (Fong et al 2014), which is known to be coincident with the kilonova/macronova candidate (Berger et al 2013;Tanvir et al 2013). Resulting GeV-TeV gamma-ray emission Murase et al 2011) and high-energy neutrino emission (Murase & Nagataki 2006;Kimura et al 2017) have also been studied.…”

Section: Introductionmentioning

confidence: 97%

Double Neutron Star Mergers and Short Gamma-ray Bursts: Long-lasting High-energy Signatures and Remnant Dichotomy

Toomey

Fang

et al. 2018

ApJ

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The recent detection of gravitational waves and electromagnetic counterparts from the double neutron star merger event GW+EM170817, supports the standard paradigm of short gamma-ray bursts (SGRBs) and kilonovae/macronovae. It is important to reveal the nature of the compact remnant left after the merger, either a black hole or neutron star, and their physical link to the origin of the long-lasting emission observed in SGRBs. The diversity of the merger remnants may also lead to different kinds of transients that can be detected in future. Here we study the high-energy emission from the long-lasting central engine left after the coalescence, under certain assumptions. In particular, we consider the X-ray emission from a remnant disk and the non-thermal nebular emission from disk-driven outflows or pulsar winds. We demonstrate that late-time X-ray and high-frequency radio emission can provide useful constraints on properties of the hidden compact remnants and their connections to long-lasting SGRB emission, and we discuss the detectability of nearby merger events through late-time observations at ∼ 30 − 100 d after the coalescence. We also investigate the GeVTeV gamma-ray emission that occurs in the presence of long-lasting central engines, and show the importance of external inverse-Compton radiation due to up-scattering of X-ray photons by relativistic electrons in the jet. We also search for high-energy gamma-rays from GW170817 in the Fermi-LAT data, and report upper limits on such long-lasting emission. Finally, we consider the implications of GW+EM170817 and discuss the constraints placed by X-ray and high-frequency radio observations.

“…Further checks whether PEs are powered by the dissipation of jet-like outflows or not may be done by detecting early-time X-ray counterparts of NS mergers without prompt γ-ray emission (Matsumoto & Kimura 2018) or searching for nebular emission formed by the central engine (Murase et al 2018). Finally, the prolonged engine activities in the PE phase can be also probed by long-lasting high-energy γ-ray and perhaps neutrino counterparts (Kimura et al 2017;Murase et al 2018;Kimura et al 2019). Table A1.…”

Section: Summary and Discussionmentioning

confidence: 99%

Linking extended and plateau emissions of short gamma-ray bursts

Matsumoto

Kimura

Monthly Notices of the Royal Astronomical Society

et al. 2020

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Some short gamma-ray bursts (SGRBs) show a longer lasting emission phase, called extended emission (EE) lasting ∼ 10 2−3 s, as well as a plateau emission (PE) lasting ∼ 10 4−5 s. While a long-lasting activity of the central engines is a promising explanation for powering both emissions, their physical origin and their emission mechanisms are still uncertain. In this work, we study the properties of the EEs and their connection with the PEs. First, we constrain the minimal Lorentz factor Γ of the outflows powering EEs, using compactness arguments and find that the outflows should be relativistic, Γ 10. We propose a consistent scenario for the PEs, where the outflow eventually catches up with the jet responsible for the prompt emission, injecting energy into the forward shock formed by the prior jet, which naturally results in a PE. We also derive the radiation efficiency of EEs and the Lorentz factor of the outflow within our scenario for 10 well-observed SGRBs accompanied by both EE and PE. The efficiency has an average value of ∼ 3 % but shows a broad distribution ranging from ∼ 0.01 to ∼ 100%. The Lorentz factor is ∼ 20 − 30, consistent with the compactness arguments. These results suggest that EEs are produced by a slower outflow via more inefficient emission than the faster outflow which causes the prompt emission with a high radiation efficiency.