{"paper":{"title":"ISM properties in hydrodynamic galaxy simulations: Turbulence cascades, cloud formation, role of gravity and feedback","arxiv_id":"1007.2566","primary_cat":"astro-ph.CO","submitted_at":"2010-07-15T14:11:29+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. 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field.","hedge":{"p":0.77,"label":"asserted"},"own_p":0.95,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.03,"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":2,"p":0.94,"id":"s2","own":true,"role":"result","text":"We show that the disk thickness is about the average Jeans scale length, and is mainly regulated by gravitational instabilities.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.93,"main_claim_p":0.18,"quantitative":true,"quantitative_p":0.67,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.94,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.06}},{"i":3,"p":0.99,"id":"s3","own":true,"role":"result","text":"From this scale of energy injection, a turbulence cascade towards small-scale is observed, with almost isotropic small-scale motions.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.94,"main_claim_p":0.08,"quantitative":false,"quantitative_p":0.09,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.99,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.01}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"result","text":"On scales larger than the disk thickness, density waves are observed, but there is also a full range of substructures with chaotic and strongly non-isotropic gas velocity dispersions.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.92,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.46,"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":0.58,"id":"s5","own":true,"role":"interpretation","text":"The power spectrum of vorticity in an LMC-sized model suggests that an inverse cascade of turbulence might be present, although energy input over a wide range of scales in the coupled gaseous+stellar fluid could also explain this quasi-2D regime on scales larger than the disk scale height.","hedge":{"p":0.86,"label":"hedged_possibility"},"own_p":0.89,"main_claim_p":0.06,"quantitative":false,"quantitative_p":0.19,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.42,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.58}},{"i":6,"p":0.96,"id":"s6","own":true,"role":"result","text":"Similar regimes of gas turbulence are also found in massive high-redshift disks with high gas fractions.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.84,"main_claim_p":0.06,"quantitative":false,"quantitative_p":0.16,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.96,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.03}},{"i":7,"p":0.61,"id":"s7","own":true,"role":"interpretation","text":"Disk properties and ISM turbulence appear to be mainly regulated by gravitational processes, both on large scales and inside dense clouds.","hedge":{"p":0.94,"label":"asserted"},"own_p":0.88,"main_claim_p":0.61,"quantitative":false,"quantitative_p":0.1,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.39,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.61}},{"i":8,"p":0.7,"id":"s8","own":true,"role":"result","text":"Star formation feedback is however essential to maintain the ISM in a steady state by balancing a systematic gas dissipation into dense and small clumps.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.82,"main_claim_p":0.14,"quantitative":false,"quantitative_p":0.06,"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":9,"p":1.0,"id":"s9","own":true,"role":"method","text":"Our galaxy simulations employ a thermal model based on a barotropic Equation of State (EoS) aimed at modelling the equilibrium of gas between various heating and cooling processes.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.84,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":1.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":10,"p":0.69,"id":"s10","own":true,"role":"method","text":"Denser gas is typically colder in this approach, which is shown to correctly reproduce the density structures of a star-forming, turbulent, unstable and cloudy ISM down to scales of a few parsecs.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.88,"main_claim_p":0.05,"quantitative":true,"quantitative_p":0.84,"role_probabilities":{"gap":0.0,"method":0.69,"result":0.29,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.01}}]},"compiled":{"main_claim":{"p":1.0,"text":"Disk properties and ISM turbulence appear to be mainly regulated by gravitational processes, 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