{"paper":{"title":"Minimal Cooling of Neutron Stars: A New Paradigm","arxiv_id":"astro-ph/0403657","primary_cat":"astro-ph","submitted_at":"2004-03-29T16:32:57+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. 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process.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.64,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.13,"role_probabilities":{"gap":0.0,"method":0.01,"result":0.0,"background":0.03,"limitation":0.0,"future_work":0.0,"contribution":0.96,"interpretation":0.0}},{"i":2,"p":0.39,"id":"s2","own":false,"role":"background","text":"This emission dominates that due to the modified Urca process for temperatures close to the critical temperature for superfluid pairing.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.25,"main_claim_p":0.03,"quantitative":true,"quantitative_p":0.93,"role_probabilities":{"gap":0.0,"method":0.05,"result":0.07,"background":0.39,"limitation":0.0,"future_work":0.0,"contribution":0.33,"interpretation":0.16}},{"i":3,"p":0.77,"id":"s3","own":false,"role":"contribution","text":"Minimal cooling is distinguished from enhanced cooling by the absence of neutrino emission from any direct Urca process, due either to nucleons or to exotica.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.24,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.48,"role_probabilities":{"gap":0.0,"method":0.06,"result":0.0,"background":0.16,"limitation":0.0,"future_work":0.0,"contribution":0.77,"interpretation":0.01}},{"i":4,"p":0.8,"id":"s4","own":true,"role":"method","text":"Within the minimal cooling scenario, theoretical cooling models can be considered to be a four parameter family involving the equation of state of dense matter, superfluid properties of dense matter, the composition of the neutron star envelope, and the mass of the neutron star.","hedge":{"p":0.9,"label":"asserted"},"own_p":0.62,"main_claim_p":0.05,"quantitative":true,"quantitative_p":0.82,"role_probabilities":{"gap":0.0,"method":0.8,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.2,"interpretation":0.0}},{"i":5,"p":0.84,"id":"s5","own":true,"role":"method","text":"Consequences of minimal cooling are explored through extensive variations of these parameters.","hedge":{"p":0.84,"label":"asserted"},"own_p":0.84,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.04,"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":6,"p":0.9,"id":"s6","own":true,"role":"method","text":"Results are compared with the inferred properties of thermally-emitting neutron stars in order to ascertain if enhanced cooling occurs in any of them.","hedge":{"p":0.65,"label":"asserted"},"own_p":0.83,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.3,"role_probabilities":{"gap":0.0,"method":0.9,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.1,"interpretation":0.0}},{"i":7,"p":0.94,"id":"s7","own":true,"role":"result","text":"All stars for which thermal emissions have been clearly detected are at least marginally consistent with the lack of enhanced cooling.","hedge":{"p":0.9,"label":"hedged_possibility"},"own_p":0.83,"main_claim_p":0.51,"quantitative":true,"quantitative_p":0.51,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.94,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.06}},{"i":8,"p":0.66,"id":"s8","own":true,"role":"result","text":"The two pulsars PSR 0833-45 (Vela) and PSR 1706-44 would require enhanced cooling in case their ages and/or temperatures are on the lower side of their estimated values whereas the four stars PSR 0656+14, PSR 1055-52, Geminga, and RX J0720.4-3125 may require some source of internal heating in case their age and/or luminosity are on the upper side of their estimated 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