{"paper":{"title":"Millisecond Pulsar Ages: Implications of Binary Evolution and a Maximum Spin Limit","arxiv_id":"0909.1562","primary_cat":"astro-ph.GA","submitted_at":"2009-09-08T20:08:56+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-1.13-20260917 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":"In the absence of constraints from the binary companion or supernova remnant, the standard method for estimating pulsar ages is to infer an age from the rate of spin-down.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.04,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.05,"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":0.89,"id":"s1","own":false,"role":"background","text":"While the generic spin-down age may give realistic estimates for normal pulsars, it can fail for pulsars with very short periods.","hedge":{"p":0.89,"label":"hedged_possibility"},"own_p":0.06,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.21,"role_probabilities":{"gap":0.06,"method":0.0,"result":0.0,"background":0.89,"limitation":0.05,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":0.96,"id":"s2","own":false,"role":"background","text":"Details of the spin-up process during the low mass X-ray binary phase pose additional constraints on the period (P) and spin-down rates (Pdot) that may consequently affect the age estimate.","hedge":{"p":0.98,"label":"hedged_possibility"},"own_p":0.07,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.12,"role_probabilities":{"gap":0.04,"method":0.0,"result":0.0,"background":0.96,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":3,"p":0.95,"id":"s3","own":true,"role":"contribution","text":"Here, we propose a new recipe to estimate millisecond pulsar (MSP) ages that parametrically incorporates constraints arising from binary evolution and limiting physics.","hedge":{"p":0.88,"label":"asserted"},"own_p":0.86,"main_claim_p":0.15,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.05,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.95,"interpretation":0.0}},{"i":4,"p":0.87,"id":"s4","own":true,"role":"result","text":"We show that the standard method can be improved by this approach to achieve age estimates closer to the true age whilst the standard spin-down age may over- or under-estimate the age of the pulsar by more than a factor of ~10 in the millisecond regime.","hedge":{"p":0.91,"label":"asserted"},"own_p":0.92,"main_claim_p":0.56,"quantitative":true,"quantitative_p":0.98,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.87,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.11,"interpretation":0.02}},{"i":5,"p":0.82,"id":"s5","own":true,"role":"contribution","text":"We use this approach to analyze the population on a broader scale.","hedge":{"p":0.76,"label":"asserted"},"own_p":0.9,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.03,"role_probabilities":{"gap":0.0,"method":0.18,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.82,"interpretation":0.0}},{"i":6,"p":0.76,"id":"s6","own":true,"role":"method","text":"For instance, in order to understand the dominant energy loss mechanism after the onset of radio emission, we test for a range of plausible braking indices.","hedge":{"p":0.47,"label":"unclear"},"own_p":0.83,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.15,"role_probabilities":{"gap":0.0,"method":0.76,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.24,"interpretation":0.0}},{"i":7,"p":1.0,"id":"s7","own":true,"role":"result","text":"We find that a braking index of n=3 is consistent with the observed MSP population.","hedge":{"p":0.86,"label":"hedged_possibility"},"own_p":0.96,"main_claim_p":0.14,"quantitative":true,"quantitative_p":0.95,"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":0.83,"id":"s8","own":true,"role":"result","text":"We demonstrate the existence and quantify the potential contributions of two main sources of age corruption: the previously known \"age bias\" due to secular acceleration and \"age contamination\" driven by sub-Eddington progenitor accretion rates.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.17,"quantitative":false,"quantitative_p":0.34,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.83,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.17,"interpretation":0.0}},{"i":9,"p":0.98,"id":"s9","own":true,"role":"result","text":"We explicitly show that descendants of LMXBs that have accreted at very low rates will exhibit ages that appear older than the age of the Galaxy.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.89,"main_claim_p":0.13,"quantitative":true,"quantitative_p":0.92,"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":10,"p":0.64,"id":"s10","own":true,"role":"contribution","text":"We further elaborate on this technique, the implications and potential solutions it offers regarding MSP evolution, the underlying age distribution and the post-accretion energy loss mechanism.","hedge":{"p":0.6,"label":"asserted"},"own_p":0.73,"main_claim_p":0.06,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.01,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.21,"contribution":0.64,"interpretation":0.14}}]},"compiled":{"main_claim":{"p":0.94,"text":"We show that the standard method can be improved by this approach to achieve age 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