{"paper":{"title":"Wave-Driven Mass Loss in the Last Year of Stellar Evolution: Setting the Stage for the Most Luminous Core-Collapse Supernovae","arxiv_id":"1202.5036","primary_cat":"astro-ph.SR","submitted_at":"2012-02-22T21:00:04+00:00","version_compiled":"v3"},"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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waves.","hedge":{"p":0.67,"label":"asserted"},"own_p":0.13,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.04,"result":0.06,"background":0.81,"limitation":0.0,"future_work":0.0,"contribution":0.04,"interpretation":0.05}},{"i":2,"p":0.73,"id":"s2","own":false,"role":"result","text":"The local wave energy flux excited by convection is itself well above Eddington during the last few years in the life of the star.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.38,"main_claim_p":0.06,"quantitative":true,"quantitative_p":0.93,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.73,"background":0.23,"limitation":0.0,"future_work":0.0,"contribution":0.03,"interpretation":0.01}},{"i":3,"p":0.76,"id":"s3","own":false,"role":"contribution","text":"We suggest that an interesting fraction of the energy in gravity waves can, in some cases, convert into sound waves as the gravity waves propagate (tunnel) towards the stellar surface.","hedge":{"p":0.66,"label":"hedged_possibility"},"own_p":0.3,"main_claim_p":0.08,"quantitative":false,"quantitative_p":0.07,"role_probabilities":{"gap":0.0,"method":0.04,"result":0.02,"background":0.01,"limitation":0.0,"future_work":0.0,"contribution":0.76,"interpretation":0.17}},{"i":4,"p":0.78,"id":"s4","own":false,"role":"result","text":"The subsequent dissipation of the sound waves can unbind up to several $M_\\odot$ of the stellar envelope.","hedge":{"p":0.92,"label":"hedged_possibility"},"own_p":0.42,"main_claim_p":0.27,"quantitative":true,"quantitative_p":0.96,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.78,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.04,"interpretation":0.18}},{"i":5,"p":0.97,"id":"s5","own":false,"role":"interpretation","text":"This wave-driven mass loss can explain the existence of extremely large stellar mass loss rates just prior to core-collapse, which are inferred via circumstellar interaction in some core-collapse supernovae (e.g., SNe 2006gy and PTF 09uj, and even Type IIn supernovae more generally).","hedge":{"p":0.69,"label":"hedged_possibility"},"own_p":0.21,"main_claim_p":0.66,"quantitative":false,"quantitative_p":0.11,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.02,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.97}},{"i":6,"p":0.72,"id":"s6","own":false,"role":"gap","text":"An outstanding question is understanding what stellar parameters (mass, rotation, metallicity, age) are the most susceptible to wave-driven mass loss.","hedge":{"p":0.49,"label":"unclear"},"own_p":0.08,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.72,"method":0.0,"result":0.0,"background":0.01,"limitation":0.01,"future_work":0.26,"contribution":0.0,"interpretation":0.0}},{"i":7,"p":0.4,"id":"s7","own":false,"role":"gap","text":"This depends on the precise internal structure of massive stars and the 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