{"paper":{"title":"Interstellar Turbulence I: Observations and Processes","arxiv_id":"astro-ph/0404451","primary_cat":"astro-ph","submitted_at":"2004-04-22T18:06:31+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-1.13.0 on the question bank abstract-p1-20260923, exactly as returned. 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sources.","hedge":{"p":0.94,"label":"asserted"},"own_p":0.15,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.11,"role_probabilities":{"gap":0.0,"method":0.13,"result":0.0,"background":0.42,"limitation":0.0,"future_work":0.01,"contribution":0.44,"interpretation":0.0}},{"i":2,"p":0.46,"id":"s2","own":false,"role":"background","text":"Turbulence theory is considered in detail, including the basic fluid equations, solenoidal and compressible modes, global inviscid quadratic invariants, scaling arguments, energy transfer and cascade, velocity probability distributions, and turbulent pressure.","hedge":{"p":0.9,"label":"asserted"},"own_p":0.1,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.17,"result":0.0,"background":0.46,"limitation":0.0,"future_work":0.0,"contribution":0.37,"interpretation":0.0}},{"i":3,"p":0.47,"id":"s3","own":false,"role":"background","text":"Theories of magnetohydrodynamic turbulence, including collisionless MHD turbulence, are discussed, emphasizing various proposals for energy spectra.","hedge":{"p":0.87,"label":"asserted"},"own_p":0.1,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.15,"result":0.0,"background":0.47,"limitation":0.0,"future_work":0.0,"contribution":0.38,"interpretation":0.0}},{"i":4,"p":0.44,"id":"s4","own":false,"role":"method","text":"A large variety of numerical simulations of interstellar turbulence are reviewed.","hedge":{"p":0.98,"label":"asserted"},"own_p":0.1,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.09,"role_probabilities":{"gap":0.0,"method":0.44,"result":0.0,"background":0.16,"limitation":0.0,"future_work":0.0,"contribution":0.4,"interpretation":0.0}},{"i":5,"p":0.76,"id":"s5","own":false,"role":"result","text":"Models have reproduced many of the basic features of the observed scaling relations, predicted fast decay rates for supersonic MHD turbulence, and derived 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