The temporal--spectral evolution of the prompt emission of gamma-ray bursts (GRBs) is simulated numerically for both leptonic and hadronic models. For weak enough magnetic fields, leptonic models can reproduce the few seconds delay of the onset of GeV photon emission observed by Fermi-LAT, due to the slow growth of the target photon field for inverse Compton scattering. However, even for stronger magnetic fields, the GeV delay can be explained with hadronic models, due to the long acceleration timescale of protons and the continuous photopion production after the end of the particle injection. While the FWHMs of the MeV and GeV lightcurves are almost the same in one-zone leptonic models, the FWHM of the 1--30 GeV lightcurves in hadronic models are significantly wider than those of the 0.1--1 MeV lightcurves. The amount of the GeV delay depends on the importance of the Klein--Nishina effect in both the leptonic and hadronic models. In our examples of hadronic models the energies of the escaped neutrons are comparable to the gamma-ray energy, although their contribution to the ultra high-energy cosmic rays is still subdominant. The resulting neutrino spectra are hard enough to avoid the flux limit constraint from IceCube. The delay of the neutrino emission onset is up to several times longer than the corresponding delay of the GeV photon emission onset. The quantitative differences in the lightcurves for various models may be further tested with future atmospheric Cherenkov telescopes whose effective area is larger than that of Fermi-LAT, such as CTA.
Delayed Wind Onset in Pa 30, the Remnant of Type Iax SN 1181
Research Center for the Early Universe (RESCEU), School of Science, The University of Tokyo（东京大学理学研究科宇宙早期研究中心）；Department of Astronomy, School of Science, The University of Tokyo（东京大学理学研究科天文学系）；Astrophysical Big Bang Laboratory, Pioneering Research Institute, RIKEN（理化学研究所先驱科学研究所天体物理大爆炸实验室）；School of Physics and Astronomy, Monash University（蒙纳士大学物理与天文学院）；Institute of Astronomy, Graduate School of Science, The University of Tokyo（东京大学大学院理学研究科天文学研究所）
Coupled Time-Dependent Proton Acceleration and Leptonic-Hadronic Radiation in Turbulent Supermassive Black Hole Coronae
Deutsches Elektronen-Synchrotron DESY（德国电子同步加速器）；National and Kapodistrian University of Athens（雅典国立卡波迪斯特里安大学）；Queen’s University（女王大学）；Arthur B. McDonald Canadian Astroparticle Physics Research Institute（阿瑟·B·麦克唐纳加拿大高能天体粒子物理研究所）；Perimeter Institute for Theoretical Physics（理论物理前沿研究所）
The Multi-Wavelength Context of Delayed Radio Emission in TDEs: Evidence for Accretion-Driven Outflows
University of Arizona（亚利桑那大学）；University of California, Berkeley（加州大学伯克利分校）；Center for Astrophysics | Harvard & Smithsonian（哈佛与史密森尼天体物理中心）；Northwestern University（西北大学）；University of Utah（犹他大学）；Radboud University（拉德堡德大学）；University of Oregon（俄勒冈大学）
Upstream neutrino production and delayed jet emission in the blazar GB6 J1542+6129
ELTE（匈牙利罗兰大学）；Konkoly Observatory, HUN-REN Research Centre for Astronomy and Earth Sciences（孔科利天文台，HUN-REN 天文学与地球科学研究中心）；CSFK, MTA Centre of Excellence（CSFK，MTA 卓越中心）；Ruhr University Bochum（波鸿鲁尔大学）；University of Florida（佛罗里达大学）；University of Szeged（塞格德大学）；Chalmers University of Technology（查尔姆斯理工大学）；Max Planck Institute for Radio Astronomy（马克斯·普朗克射电天文研究所）；University of Alabama（阿拉巴马大学）
