{"paper":{"title":"Nonthermal afterglow of the binary neutron star merger GW170817: a more natural modeling of electron energy distribution leads to a qualitatively different new solution","arxiv_id":"1810.02587","primary_cat":"astro-ph.HE","submitted_at":"2018-10-05T09:47:01+00:00","version_compiled":"v2"},"notice":"Every quoted sentence is the authors' text from the arXiv listing abstract. Labels and probabilities are the outputs of classifier-1.13.0 on the question bank abstract-p1-20260923, exactly as returned. No sentence in this record was written by a language model.","schema":"pith.compiled-record/v0","status":"compiled","abstract":{"source":"arXiv listing abstract v2","sentences":[{"i":0,"p":0.98,"id":"s0","own":false,"role":"background","text":"The observed nonthermal afterglow spectrum of the binary neutron star (BNS) merger GW170817 from radio to X-ray are consistent with synchrotron radiation by shock-accelerated electrons.","hedge":{"p":0.9,"label":"hedged_possibility"},"own_p":0.11,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.11,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.02,"background":0.98,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":1,"p":0.51,"id":"s1","own":false,"role":"gap","text":"However, previous afterglow modeling studies were based on a simplified assumption that the acceleration efficiency is extremely high, i.e. all electrons in the shock are accelerated as a nonthermal population.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.04,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.32,"role_probabilities":{"gap":0.51,"method":0.0,"result":0.0,"background":0.47,"limitation":0.02,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":0.83,"id":"s2","own":false,"role":"background","text":"This affects the estimate of the minimum electron energy and hence $\\nu_m$, the peak frequency of the afterglow spectrum.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.08,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.06,"method":0.0,"result":0.0,"background":0.83,"limitation":0.01,"future_work":0.0,"contribution":0.0,"interpretation":0.1}},{"i":3,"p":0.53,"id":"s3","own":true,"role":"contribution","text":"Here we present Bayesian fitting to the observed data with a more natural electron energy distribution, in which the acceleration efficiency is a free parameter.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.95,"main_claim_p":0.09,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.47,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.53,"interpretation":0.0}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"result","text":"Interestingly, the maximum likelihood solutions are found with radio flux below $\\nu_m$ in the early phase, in contrast to previous studies that found the radio frequency always above $\\nu_m$.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.93,"main_claim_p":0.43,"quantitative":true,"quantitative_p":0.9,"role_probabilities":{"gap":0.0,"method":0.0,"result":1.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":5,"p":0.96,"id":"s5","own":true,"role":"interpretation","text":"Therefore the $\\nu_m$ passage through the radio band could have been clearly detected for GW170817, if sufficient low-frequency radio data had been taken in early time.","hedge":{"p":1.0,"label":"hedged_possibility"},"own_p":0.6,"main_claim_p":0.18,"quantitative":false,"quantitative_p":0.1,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.01,"background":0.0,"limitation":0.0,"future_work":0.03,"contribution":0.0,"interpretation":0.96}},{"i":6,"p":1.0,"id":"s6","own":true,"role":"result","text":"In the new solutions, the lowest energy of electrons is found close to equipartition with the post shock protons, but only a small fraction ($<$10\\%) of electrons are accelerated as nonthermal particles.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.26,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":1.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":7,"p":1.0,"id":"s7","own":true,"role":"result","text":"The jet energy and interstellar medium density are increased by 1--2 orders of magnitude from the conventional modeling, though these are still consistent with other constraints.","hedge":{"p":0.97,"label":"asserted"},"own_p":0.9,"main_claim_p":0.12,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":1.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":8,"p":1.0,"id":"s8","own":false,"role":"future_work","text":"We encourage to take densely sampled low-frequency radio data in the early phase for future BNS merger events, which would potentially detect $\\nu_m$ passage and give a strong constraint on electron energy distribution and particle acceleration 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