{"paper":{"title":"Unified interpretation of cosmic-ray nuclei and antiproton recent measurements","arxiv_id":"0909.4548","primary_cat":"astro-ph.HE","submitted_at":"2009-09-25T10:22:41+00:00","version_compiled":"v4"},"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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model.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.87,"main_claim_p":0.61,"quantitative":false,"quantitative_p":0.14,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.93,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.07,"interpretation":0.0}},{"i":2,"p":0.7,"id":"s2","own":true,"role":"result","text":"The requirement that light nuclei and $\\bar p$ data are consistently reproduced within experimental uncertainties places significant limits on the main propagation parameters.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.72,"main_claim_p":0.29,"quantitative":false,"quantitative_p":0.23,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.7,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.3}},{"i":3,"p":1.0,"id":"s3","own":true,"role":"result","text":"In particular, we find the allowed range of the diffusion coefficient spectral index to be $0.3 < \\delta < 0.6$ at 95% confidence level and that Kraichnan type diffusion is favored with respect to Kolmogorov.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.96,"main_claim_p":0.28,"quantitative":true,"quantitative_p":0.99,"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":"result","text":"While some amount of reacceleration is required, only a limited range of the Alfv\\'en velocity value ($10 \\simleq v_A \\simleq 20 \\km \\s^{-1}$) is allowed by a combined analysis of nuclear and antiproton data, which we perform here for the first time.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.94,"main_claim_p":0.19,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.99,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.0}},{"i":5,"p":0.83,"id":"s5","own":true,"role":"result","text":"If antiproton data are not used to constrain the propagation parameters, a larger set of models is allowed.","hedge":{"p":0.89,"label":"asserted"},"own_p":0.64,"main_claim_p":0.06,"quantitative":false,"quantitative_p":0.21,"role_probabilities":{"gap":0.01,"method":0.01,"result":0.83,"background":0.0,"limitation":0.03,"future_work":0.0,"contribution":0.01,"interpretation":0.11}},{"i":6,"p":0.57,"id":"s6","own":true,"role":"method","text":"In this case, we determine which combinations of the relevant parameters maximize and minimize the antiproton flux under the condition of still fitting light nuclei data at 95% C.L.","hedge":{"p":0.98,"label":"asserted"},"own_p":0.93,"main_claim_p":0.05,"quantitative":true,"quantitative_p":0.79,"role_probabilities":{"gap":0.0,"method":0.57,"result":0.06,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.36,"interpretation":0.01}},{"i":7,"p":0.74,"id":"s7","own":false,"role":"interpretation","text":"These models may then be used to constrain a possible extra antiproton 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