{"paper":{"title":"Intra-Binary Shock Heating of Black Widow Companions","arxiv_id":"1606.03518","primary_cat":"astro-ph.HE","submitted_at":"2016-06-11T01:22:06+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":"The low mass companions of evaporating binary pulsars (black widows and their ilk) are strongly heated on the side facing the pulsar.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.14,"main_claim_p":0.06,"quantitative":false,"quantitative_p":0.06,"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":0.57,"id":"s1","own":false,"role":"gap","text":"However in high-quality photometric and spectroscopic data the heating pattern does not match that expected for direct pulsar illumination.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.43,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.29,"role_probabilities":{"gap":0.57,"method":0.0,"result":0.01,"background":0.42,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":0.93,"id":"s2","own":true,"role":"contribution","text":"Here we explore heating mediated by an intra-binary shock (IBS).","hedge":{"p":0.44,"label":"asserted"},"own_p":0.76,"main_claim_p":0.08,"quantitative":false,"quantitative_p":0.03,"role_probabilities":{"gap":0.0,"method":0.07,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.93,"interpretation":0.0}},{"i":3,"p":0.95,"id":"s3","own":true,"role":"method","text":"We develop a simple analytic model and implement it in the popular `ICARUS' light curve code.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.96,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.95,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.05,"interpretation":0.0}},{"i":4,"p":0.99,"id":"s4","own":true,"role":"method","text":"The model is parameterized by the wind momentum ratio beta and velocity v_Rel v_orb and assumes that the reprocessed pulsar wind emits prompt particles or radiation to heat the companion surface.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.82,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.08,"role_probabilities":{"gap":0.0,"method":0.99,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.0}},{"i":5,"p":0.77,"id":"s5","own":true,"role":"result","text":"We illustrate an interesting range of light curve asymmetries controlled by these parameters.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.9,"main_claim_p":0.06,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.03,"result":0.77,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.19,"interpretation":0.01}},{"i":6,"p":0.63,"id":"s6","own":true,"role":"method","text":"The code also computes the IBS synchrotron emission pattern, and thus can model black widow X-ray light curves.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.87,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.63,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.37,"interpretation":0.0}},{"i":7,"p":0.98,"id":"s7","own":true,"role":"result","text":"As a test we apply the results to the high quality asymmetric optical light curves of PSR J2215+5135; the resulting fit gives a substantial improvement upon direct heating models and produces an X-ray light curve consistent with that seen.","hedge":{"p":0.91,"label":"asserted"},"own_p":0.95,"main_claim_p":0.52,"quantitative":true,"quantitative_p":0.82,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.98,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.02,"interpretation":0.0}},{"i":8,"p":0.57,"id":"s8","own":true,"role":"interpretation","text":"The IBS model parameters imply that, at the present loss rate, the companion evaporation has a characteristic timescale tau_evap ~150My.","hedge":{"p":0.8,"label":"asserted"},"own_p":0.91,"main_claim_p":0.22,"quantitative":true,"quantitative_p":0.98,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.43,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.57}},{"i":9,"p":1.0,"id":"s9","own":true,"role":"limitation","text":"Still, the model is not fully satisfactory, indicating additional unmodeled physical effects.","hedge":{"p":0.94,"label":"asserted"},"own_p":0.82,"main_claim_p":0.08,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":1.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}}]},"compiled":{"main_claim":{"p":0.99,"text":"As a test we apply the results to the high quality asymmetric optical light curves of PSR J2215+5135; 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