{"paper":{"title":"Constraining the FRB Central Engine from Flux Variations of Persistent Radio Sources: FRB 20240114A as the First Attempt","arxiv_id":"2610.27489","primary_cat":"astro-ph.HE","submitted_at":"2026-10-20T02:01:39+00:00","version_compiled":"v1"},"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 v1","sentences":[{"i":0,"p":1.0,"id":"s0","own":false,"role":"background","text":"Some repeating fast radio bursts (FRBs) are associated with persistent radio sources (PRSs), likely driven by the long-term activity of a central engine.","hedge":{"p":0.92,"label":"hedged_possibility"},"own_p":0.04,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":1.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":1,"p":0.99,"id":"s1","own":true,"role":"contribution","text":"We investigate FRB 20240114A-currently the most active repeating FRB-to explore the link between its burst activity and the flux variability of its associated PRS.","hedge":{"p":0.75,"label":"asserted"},"own_p":0.79,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.37,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.01,"limitation":0.0,"future_work":0.0,"contribution":0.99,"interpretation":0.0}},{"i":2,"p":0.98,"id":"s2","own":true,"role":"method","text":"We model electrons responsible for FRB emission being continuously injected from a central magnetar into its magnetar wind nebula (MWN), where synchrotron radiation produces the PRS.","hedge":{"p":0.82,"label":"asserted"},"own_p":0.52,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.03,"role_probabilities":{"gap":0.0,"method":0.98,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.02,"interpretation":0.0}},{"i":3,"p":0.84,"id":"s3","own":true,"role":"method","text":"Comparing our model with the latest PRS spectra and flux variations, we constrain the physical properties of the FRB source.","hedge":{"p":0.98,"label":"asserted"},"own_p":0.94,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.11,"role_probabilities":{"gap":0.0,"method":0.84,"result":0.01,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.15,"interpretation":0.0}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"result","text":"We find that the total energy injected into the MWN during FAST observations from January to August 2024 is $\\sim 10^{48} \\, \\rm{erg}$, consistent with the magnetic energy budget of a magnetar with an internal magnetic field of $\\sim 10^{16} \\, \\rm G$.","hedge":{"p":0.94,"label":"asserted"},"own_p":0.96,"main_claim_p":0.25,"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":5,"p":0.98,"id":"s5","own":true,"role":"result","text":"The bulk Lorentz factor of the FRB-emitting plasma is mildly constrained to $\\lesssim 10^3$, and FRB 20240114A is inferred to be powered by a young magnetar aged $\\sim 10$-$20 \\, \\rm {yr}$.","hedge":{"p":0.81,"label":"asserted"},"own_p":0.95,"main_claim_p":0.24,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.98,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.02}},{"i":6,"p":0.98,"id":"s6","own":true,"role":"interpretation","text":"These results show that the PRS flux variability effectively probes FRB emission properties.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.82,"main_claim_p":0.56,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.02,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.98}},{"i":7,"p":0.46,"id":"s7","own":true,"role":"result","text":"We predict that while PRS luminosity increases rapidly with enhanced FRB activity, it will slowly fade over decades via adiabatic cooling after FRB activity ceases.","hedge":{"p":0.54,"label":"asserted"},"own_p":0.75,"main_claim_p":0.13,"quantitative":false,"quantitative_p":0.26,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.46,"background":0.0,"limitation":0.0,"future_work":0.09,"contribution":0.03,"interpretation":0.42}},{"i":8,"p":0.51,"id":"s8","own":true,"role":"interpretation","text":"Energetics suggest that the hyper-active phase observed in FRB 20240114A (burst rate $\\sim 700 \\, \\rm hr^{-1}$) is a rare state with a duty cycle of $\\lesssim 10^{-2}$, which is broadly consistent with its detection rate in current FRB-PRS samples.","hedge":{"p":0.87,"label":"hedged_possibility"},"own_p":0.87,"main_claim_p":0.13,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.49,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.51}}]},"compiled":{"main_claim":{"p":0.95,"text":"These results show that the PRS flux 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