{"paper":{"title":"Hall drift in the crust of neutron stars - necessary for radio pulsar activity?","arxiv_id":"1206.1790","primary_cat":"astro-ph.SR","submitted_at":"2012-06-08T15:15:24+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":"The radio pulsar models based on the existence of an inner accelerating gap located above the polar cap rely on the existence of a small scale, strong surface magnetic field $B_s$.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.05,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.07,"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":1.0,"id":"s1","own":false,"role":"background","text":"This field exceeds the dipolar field $B_d$, responsible for the braking of the pulsar rotation, by at least one order of magnitude.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.09,"main_claim_p":0.03,"quantitative":true,"quantitative_p":0.99,"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":0.58,"id":"s2","own":false,"role":"gap","text":"Neither magnetospheric currents nor small scale field components generated during neutron star's birth can provide such field structures in old pulsars.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.15,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.19,"role_probabilities":{"gap":0.58,"method":0.0,"result":0.01,"background":0.41,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":3,"p":0.74,"id":"s3","own":false,"role":"background","text":"While the former are too weak to create $B_s \\gtrsim 5\\times 10^{13}$G$\\;\\gg B_d$, the ohmic decay time of the latter is much shorter than $10^6$ years.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.15,"main_claim_p":0.03,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.24,"method":0.0,"result":0.01,"background":0.74,"limitation":0.01,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":4,"p":0.87,"id":"s4","own":false,"role":"contribution","text":"We suggest that a large amount of magnetic energy is stored in a toroidal field component that is confined in deeper layers of the crust, where the ohmic decay time exceeds $10^7$ years.","hedge":{"p":0.87,"label":"hedged_possibility"},"own_p":0.32,"main_claim_p":0.18,"quantitative":true,"quantitative_p":0.97,"role_probabilities":{"gap":0.05,"method":0.02,"result":0.01,"background":0.03,"limitation":0.0,"future_work":0.0,"contribution":0.87,"interpretation":0.02}},{"i":5,"p":0.67,"id":"s5","own":false,"role":"background","text":"This toroidal field may be created by various processes acting early in a neutron star's life.","hedge":{"p":0.99,"label":"hedged_possibility"},"own_p":0.14,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.04,"method":0.07,"result":0.01,"background":0.67,"limitation":0.0,"future_work":0.0,"contribution":0.14,"interpretation":0.07}},{"i":6,"p":0.56,"id":"s6","own":false,"role":"contribution","text":"The Hall drift is a non-linear mechanism that, due to the coupling between different components and scales, may be able to create the demanded strong, small scale, magnetic spots.","hedge":{"p":1.0,"label":"hedged_possibility"},"own_p":0.13,"main_claim_p":0.21,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.03,"method":0.12,"result":0.0,"background":0.27,"limitation":0.0,"future_work":0.0,"contribution":0.56,"interpretation":0.02}},{"i":7,"p":0.98,"id":"s7","own":true,"role":"result","text":"Taking into account both realistic crustal microphysics and a minimal cooling scenario, we show that, in axial symmetry, these field structures are created on a Hall time scale of $10^3$-$10^4$ years.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.94,"main_claim_p":0.4,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.98,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.02,"interpretation":0.0}},{"i":8,"p":0.79,"id":"s8","own":true,"role":"interpretation","text":"These magnetic spots can be long-lived, thereby fulfilling the pre-conditions for the appearance of the radio pulsar activity.","hedge":{"p":0.61,"label":"hedged_possibility"},"own_p":0.57,"main_claim_p":0.4,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.21,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.79}},{"i":9,"p":0.6,"id":"s9","own":false,"role":"interpretation","text":"Such magnetic structures created by the Hall drift are not static, and dynamical variations on the Hall time 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