{"paper":{"title":"Antiproton Flux in Cosmic Ray Propagation Models with Anisotropic Diffusion","arxiv_id":"1012.0587","primary_cat":"astro-ph.HE","submitted_at":"2010-12-02T21:42:36+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-1.13-20260917 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":"Recently a cosmic ray propagation model has been introduced, where anisotropic diffusion is used as a mechanism to allow for $\\mathcal{O}(100)$ km/s galactic winds.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.06,"main_claim_p":0.03,"quantitative":true,"quantitative_p":0.92,"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":0.74,"id":"s1","own":false,"role":"background","text":"This model predicts a reduced antiproton background flux, suggesting an excess is being observed.","hedge":{"p":0.94,"label":"hedged_possibility"},"own_p":0.09,"main_claim_p":0.17,"quantitative":false,"quantitative_p":0.14,"role_probabilities":{"gap":0.01,"method":0.0,"result":0.09,"background":0.74,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.16}},{"i":2,"p":0.93,"id":"s2","own":true,"role":"method","text":"We implement this model in GALPROP v50.1 and perform a $\\chi^2$ analysis for B/C, $^{10}$Be/$^{9}$Be, and the recent PAMELA $\\bar{p}/p$ datasets.","hedge":{"p":0.97,"label":"asserted"},"own_p":0.95,"main_claim_p":0.05,"quantitative":true,"quantitative_p":0.81,"role_probabilities":{"gap":0.0,"method":0.93,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.07,"interpretation":0.0}},{"i":3,"p":0.83,"id":"s3","own":true,"role":"result","text":"By introducing a power-index parameter $\\alpha$ that dictates the dependence of the diffusion coefficient $D_{xx}$ on height $|z|$ away from the galactic plane, we confirm that isotropic diffusion models with $\\alpha=0$ cannot accommodate high velocity convective winds suggested by ROSAT, while models with $\\alpha=1$ ($D_{xx}\\propto |z|$) can give a very good fit.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.93,"main_claim_p":0.34,"quantitative":true,"quantitative_p":0.94,"role_probabilities":{"gap":0.0,"method":0.12,"result":0.83,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.04,"interpretation":0.01}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"result","text":"A fit to B/C and $^{10}$Be/$^{9}$Be data predicts a lower $\\bar{p}/p$ flux ratio than the PAMELA measurement at energies between approximately 2 GeV to 20 GeV.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.9,"main_claim_p":0.3,"quantitative":true,"quantitative_p":0.98,"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":5,"p":0.62,"id":"s5","own":true,"role":"interpretation","text":"A combined fit including in addition the $\\bar{p}/p$ data is marginal, suggesting only a partial contribution to the measured antiproton flux.","hedge":{"p":0.98,"label":"hedged_possibility"},"own_p":0.92,"main_claim_p":0.45,"quantitative":false,"quantitative_p":0.19,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.38,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.62}}]},"compiled":{"main_claim":{"p":0.89,"text":"A combined fit including in addition the $\\bar{p}/p$ data is marginal, suggesting only a partial contribution to the measured antiproton flux.","location":"abstract 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