{"paper":{"title":"From Neutrino- to Photon-Cooled in Three Years: Can Fallback Accretion Explain the X-ray Excess in GW170817?","arxiv_id":"2106.02052","primary_cat":"astro-ph.HE","submitted_at":"2021-06-03T18:00:04+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":"An excess in the X-ray emission from the neutron star merger GW170817 above the predicted afterglow was recently detected t~3.4 years post-merger.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.15,"main_claim_p":0.03,"quantitative":true,"quantitative_p":0.96,"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":0.92,"id":"s1","own":false,"role":"background","text":"One possible origin for the excess is accretion onto the newly unshrouded black hole (BH) remnant.","hedge":{"p":1.0,"label":"hedged_possibility"},"own_p":0.07,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.03,"role_probabilities":{"gap":0.01,"method":0.0,"result":0.0,"background":0.92,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.06}},{"i":2,"p":0.52,"id":"s2","own":false,"role":"background","text":"While fall-back of the bound dynamical ejecta is insufficient to generate the excess luminosity, L_X ~ 5e38 erg/s, fall-back from the disk wind ejecta-due to their larger mass and lower velocity-remains a viable possibility.","hedge":{"p":0.75,"label":"hedged_possibility"},"own_p":0.33,"main_claim_p":0.2,"quantitative":true,"quantitative_p":0.98,"role_probabilities":{"gap":0.1,"method":0.0,"result":0.28,"background":0.52,"limitation":0.01,"future_work":0.0,"contribution":0.01,"interpretation":0.08}},{"i":3,"p":0.85,"id":"s3","own":true,"role":"method","text":"We present hydrodynamic alpha-viscosity simulations of the post-merger disk evolution which extend to an unprecedently long timescale t ~ 35 s post-merger, as necessary to capture the end of photodissociation and the asymptotic evolution into the radiatively inefficient regime.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.04,"quantitative":true,"quantitative_p":0.97,"role_probabilities":{"gap":0.0,"method":0.85,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.15,"interpretation":0.0}},{"i":4,"p":0.88,"id":"s4","own":true,"role":"result","text":"Due to inefficient neutrino cooling, the BH accretion rate decays rapidly at late times (Mdot_BH ~ t^(-\\beta_BH), where \\beta_BH ~ 2.4-2.8), seemingly incompatible with generating the late-time excess.","hedge":{"p":0.97,"label":"asserted"},"own_p":0.66,"main_claim_p":0.04,"quantitative":true,"quantitative_p":0.98,"role_probabilities":{"gap":0.03,"method":0.0,"result":0.88,"background":0.03,"limitation":0.04,"future_work":0.0,"contribution":0.0,"interpretation":0.02}},{"i":5,"p":1.0,"id":"s5","own":true,"role":"result","text":"However, the rate at which matter falls back to the inner disk from the equatorial regions (as inferred by the rate matter is unbound in outflows by viscous heating at higher latitudes) decays more gradually, Mdot_fb ~ t^(-\\beta_fb) with \\beta_fb ~ 1.43 in our alpha ~ 0.03 simulations.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.93,"main_claim_p":0.1,"quantitative":true,"quantitative_p":0.98,"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":6,"p":0.77,"id":"s6","own":true,"role":"result","text":"By the present epoch, the fall-back rate has become sub-Eddington and the disk can again accrete efficiently, i.e. Mdot_BH ~ Mdot_fb, this time as a result of photon cooling instead of neutrino cooling.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.79,"main_claim_p":0.22,"quantitative":true,"quantitative_p":0.51,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.77,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.23}},{"i":7,"p":0.6,"id":"s7","own":true,"role":"result","text":"The predicted X-ray accretion luminosity at the present epoch is L_X ~ 0.1 Mdot_BH c^2 ~ (2-70)e38 erg/s for beta_FB ~ 1.43-1.66, thus supporting (with caveats) an accretion-powered origin for the X-ray excess in GW170817.","hedge":{"p":0.94,"label":"hedged_possibility"},"own_p":0.89,"main_claim_p":0.83,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.6,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.4}},{"i":8,"p":0.93,"id":"s8","own":true,"role":"interpretation","text":"The suppressed BH accretion rate prior to the radiatively efficient (sub-Eddington) transition, weeks to months after the merger, is key to avoid overproducing the kilonova luminosity via reprocessing.","hedge":{"p":0.98,"label":"asserted"},"own_p":0.6,"main_claim_p":0.09,"quantitative":false,"quantitative_p":0.32,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.07,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.93}}]},"compiled":{"main_claim":{"p":1.0,"text":"The predicted X-ray accretion luminosity at the present epoch is L_X ~ 0.1 Mdot_BH c^2 ~ (2-70)e38 erg/s for beta_FB ~ 1.43-1.66, 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