{"paper":{"title":"Binaries migrating in a gaseous disk: Where are the Galactic center binaries?","arxiv_id":"1011.0360","primary_cat":"astro-ph.GA","submitted_at":"2010-11-01T15:56:51+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":0.99,"id":"s0","own":false,"role":"background","text":"The massive stars in the Galactic center inner arcsecond share analogous properties with the so-called Hot Jupiters.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.18,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.47,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.99,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.01}},{"i":1,"p":1.0,"id":"s1","own":false,"role":"background","text":"Most of these young stars have highly eccentric orbits, and were probably not formed in-situ.","hedge":{"p":0.74,"label":"hedged_possibility"},"own_p":0.14,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.24,"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":2,"p":1.0,"id":"s2","own":false,"role":"background","text":"It has been proposed that these stars acquired their current orbits from the tidal disruption of compact massive binaries scattered toward the proximity of the central supermassive black hole.","hedge":{"p":0.74,"label":"hedged_possibility"},"own_p":0.03,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.05,"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":3,"p":0.87,"id":"s3","own":true,"role":"contribution","text":"Assuming a binary star formed in a thin gaseous disk beyond 0.1 pc from the central object, we investigate the relevance of disk-satellite interactions to harden the binding energy of the binary, and to drive its inward migration.","hedge":{"p":0.31,"label":"asserted"},"own_p":0.59,"main_claim_p":0.05,"quantitative":true,"quantitative_p":0.92,"role_probabilities":{"gap":0.0,"method":0.13,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.87,"interpretation":0.0}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"result","text":"A massive, equal-mass binary star is found to become more tightly wound as it migrates inwards toward the central black hole.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.91,"main_claim_p":0.26,"quantitative":false,"quantitative_p":0.11,"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":1.0,"id":"s5","own":true,"role":"result","text":"The migration timescale is very similar to that of a single-star satellite of the same mass.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.8,"main_claim_p":0.11,"quantitative":true,"quantitative_p":0.91,"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":6,"p":0.75,"id":"s6","own":true,"role":"result","text":"The binary's hardening is caused by the formation of spiral tails lagging the stars inside the binary's Hill radius.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.83,"main_claim_p":0.15,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.75,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.25}},{"i":7,"p":0.98,"id":"s7","own":true,"role":"result","text":"We show that the hardening timescale is mostly determined by the mass of gas inside the binary's Hill radius, and that it is much shorter than the migration timescale.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.92,"main_claim_p":0.31,"quantitative":true,"quantitative_p":0.96,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.98,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.02}},{"i":8,"p":0.85,"id":"s8","own":false,"role":"interpretation","text":"We discuss some implications of the binary's hardening process.","hedge":{"p":0.97,"label":"unclear"},"own_p":0.38,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.02,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.1,"contribution":0.05,"interpretation":0.85}},{"i":9,"p":0.84,"id":"s9","own":false,"role":"interpretation","text":"When the more massive (primary) components of close binaries eject most their mass through supernova explosion, their secondary stars may attain a range of eccentricities and inclinations.","hedge":{"p":1.0,"label":"hedged_possibility"},"own_p":0.11,"main_claim_p":0.08,"quantitative":false,"quantitative_p":0.14,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.12,"background":0.03,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.84}},{"i":10,"p":1.0,"id":"s10","own":false,"role":"interpretation","text":"Such processes may provide an alternative unified scenario for the origin of the kinematic properties of the central cluster and S-stars in the Galactic center as well as the high velocity stars in the Galactic halo.","hedge":{"p":1.0,"label":"hedged_possibility"},"own_p":0.15,"main_claim_p":0.32,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":1.0}}]},"compiled":{"main_claim":{"p":0.67,"text":"Such processes may provide an alternative unified scenario for the origin of the kinematic 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