{"paper":{"title":"Population synthesis of Be X-ray binaries: metallicity dependence of total X-ray outputs","arxiv_id":"2308.06154","primary_cat":"astro-ph.HE","submitted_at":"2023-08-11T14:33:07+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":1.0,"id":"s0","own":false,"role":"background","text":"X-ray binaries (XRBs) are thought to regulate cosmic thermal and ionization histories during the Epoch of Reionization and Cosmic Dawn ($z\\sim 5-30$).Theoretical predictions of the X-ray emission from XRBs are important for modelling such early cosmic evolution.","hedge":{"p":0.85,"label":"hedged_possibility"},"own_p":0.04,"main_claim_p":0.02,"quantitative":true,"quantitative_p":0.81,"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":1.0,"id":"s1","own":false,"role":"gap","text":"Nevertheless, the contribution from Be-XRBs, powered by accretion of compact objects from decretion disks around rapidly rotating O/B stars, has not been investigated systematically.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.07,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":1.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":0.91,"id":"s2","own":false,"role":"background","text":"Be-XRBs are the largest class of high-mass XRBs (HMXBs) identified in local observations and are expected to play even more important roles in metal-poor environments at high redshifts.","hedge":{"p":0.56,"label":"hedged_possibility"},"own_p":0.07,"main_claim_p":0.05,"quantitative":true,"quantitative_p":0.6,"role_probabilities":{"gap":0.08,"method":0.0,"result":0.0,"background":0.91,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.01}},{"i":3,"p":0.84,"id":"s3","own":true,"role":"method","text":"In light of this, we build a physically motivated model for Be-XRBs based on recent hydrodynamic simulations and observations of decretion disks.","hedge":{"p":0.98,"label":"asserted"},"own_p":0.94,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.03,"role_probabilities":{"gap":0.0,"method":0.84,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.16,"interpretation":0.0}},{"i":4,"p":0.46,"id":"s4","own":true,"role":"result","text":"Our model is able to reproduce the observed population of Be-XRBs in the Small Magellanic Cloud with appropriate initial conditions and binary stellar evolution parameters.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.96,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.07,"role_probabilities":{"gap":0.0,"method":0.37,"result":0.46,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.16,"interpretation":0.01}},{"i":5,"p":0.85,"id":"s5","own":true,"role":"method","text":"We derive the X-ray output from Be-XRBs as a function of metallicity in the (absolute) metallicity range $Z\\in [10^{-4},0.03]$ with a large suite of binary population synthesis (BPS) simulations.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.97,"main_claim_p":0.04,"quantitative":true,"quantitative_p":0.95,"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":6,"p":1.0,"id":"s6","own":true,"role":"result","text":"The simulated Be-XRBs can explain a non-negligible fraction ($\\gtrsim 30\\%$) of the total X-ray output from HMXBs observed in nearby galaxies for $Z\\sim 0.0003-0.02$.","hedge":{"p":0.79,"label":"asserted"},"own_p":0.92,"main_claim_p":0.17,"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":0.99,"id":"s7","own":true,"role":"result","text":"The X-ray luminosity per unit star formation rate from Be-XRBs in our fiducial model increases by a factor of $\\sim 8$ from $Z=0.02$ to $Z=0.0003$, which is similar to the trend seen in observations of all types of HMXBs.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.17,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.99,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.01}},{"i":8,"p":0.5,"id":"s8","own":false,"role":"interpretation","text":"We conclude that Be-XRBs are potentially important X-ray sources that deserve greater attention in BPS of XRBs.","hedge":{"p":0.99,"label":"hedged_possibility"},"own_p":0.45,"main_claim_p":0.94,"quantitative":false,"quantitative_p":0.03,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.5,"contribution":0.0,"interpretation":0.5}}]},"compiled":{"main_claim":{"p":0.99,"text":"We conclude that Be-XRBs are potentially important X-ray sources that deserve greater attention in BPS of 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