{"paper":{"title":"The observed neutron star mass distribution as a probe of the supernova explosion mechanism","arxiv_id":"1204.5478","primary_cat":"astro-ph.SR","submitted_at":"2012-04-24T20:00:04+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. 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formation.","hedge":{"p":0.96,"label":"asserted"},"own_p":0.96,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.25,"role_probabilities":{"gap":0.0,"method":0.4,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.6,"interpretation":0.0}},{"i":2,"p":1.0,"id":"s2","own":true,"role":"result","text":"We find that models with standard binary mass ratio distributions are strongly preferred over independently picking the masses from the initial mass function, although the strength of the inference depends on whether current assumptions for identifying the remnants of the primary and secondary stars are correct.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.96,"main_claim_p":0.19,"quantitative":true,"quantitative_p":0.8,"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":3,"p":1.0,"id":"s3","own":true,"role":"result","text":"Second, NS formation models with no mass fallback are favored because they reduce the dispersion in NS masses.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.9,"main_claim_p":0.13,"quantitative":true,"quantitative_p":0.5,"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":4,"p":0.99,"id":"s4","own":true,"role":"interpretation","text":"The double NS system masses thus directly point to the mass coordinate where the supernova explosion was initiated, making them an excellent probe of the supernova explosion mechanism.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.69,"main_claim_p":0.63,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.01,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.99}},{"i":5,"p":0.98,"id":"s5","own":true,"role":"result","text":"If we assume no fallback and simply vary the mass coordinate separating the remnant and the supernova ejecta, we find that for solar metallicity stars the explosion most likely develops at the edge of the iron core at a specific entropy of about 2.8 k_B.","hedge":{"p":0.62,"label":"hedged_possibility"},"own_p":0.95,"main_claim_p":0.23,"quantitative":true,"quantitative_p":0.98,"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":1.0,"id":"s6","own":false,"role":"limitation","text":"The primary limitations of our study are the poor knowledge of the supernova explosion mechanism and the lack of broad range of SN model explosions of LMC to solar 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