{"paper":{"title":"Strange mode instability for micro-variations in Luminous Blue Variables","arxiv_id":"1305.4728","primary_cat":"astro-ph.SR","submitted_at":"2013-05-21T06:38:19+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":"If a massive star has lost significant mass during its red-supergiant stage, it would return to blue region in the HR diagram and spend a part of the core-He burning stage as a blue supergiant having a luminosity to mass ratio (L/M) considerably larger than about 10^4 (in solar units); the duration depends on the degree of internal mixing and on the metallicity.","hedge":{"p":0.5,"label":"hedged_possibility"},"own_p":0.08,"main_claim_p":0.07,"quantitative":true,"quantitative_p":0.98,"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":0.84,"id":"s1","own":false,"role":"background","text":"Then, various stellar pulsations are excited by enhanced \\kappa-mechanism and strange mode instability.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.13,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.04,"result":0.06,"background":0.84,"limitation":0.0,"future_work":0.0,"contribution":0.03,"interpretation":0.03}},{"i":2,"p":0.5,"id":"s2","own":true,"role":"method","text":"Assuming these pulsations to be responsible for (at least some of) the quasi-periodic light and radial-velocity variations in \\alpha Cygni variables including luminous blue variables (LBVs; or S Dor variables), we can predict masses and surface compositions for these variables, and compare them with observed ones to constrain the evolutionary models.","hedge":{"p":0.79,"label":"hedged_possibility"},"own_p":0.5,"main_claim_p":0.09,"quantitative":false,"quantitative_p":0.1,"role_probabilities":{"gap":0.0,"method":0.5,"result":0.0,"background":0.01,"limitation":0.0,"future_work":0.0,"contribution":0.45,"interpretation":0.04}},{"i":3,"p":0.55,"id":"s3","own":true,"role":"method","text":"We discuss radial pulsations excited in evolutionary models of an initial mass of 40 M_\\odot with solar metallicity of Z=0.014, and compare them to micro-variations in the two Galactic LBVs, HR Car and HD 160529.","hedge":{"p":0.89,"label":"asserted"},"own_p":0.9,"main_claim_p":0.05,"quantitative":true,"quantitative_p":0.96,"role_probabilities":{"gap":0.0,"method":0.55,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.45,"interpretation":0.0}},{"i":4,"p":0.99,"id":"s4","own":true,"role":"result","text":"We have found that these stars should has lost more than half of the initial mass and their surface CNO abundances should be significantly modified from the original ones showing partial H-burning products.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.93,"main_claim_p":0.79,"quantitative":true,"quantitative_p":0.97,"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}}]},"compiled":{"main_claim":{"p":1.0,"text":"We have found that these stars should has lost more than half of the initial mass and their surface CNO abundances should be significantly modified from the original ones showing partial H-burning products.","location":"abstract s4","hedge_strength":{"p":0.99,"label":"asserted"}},"provenance":{"route":{"via":"OpenRouter","model":"classifier-1.13","endpoint":"https://openrouter.ai/api/v1/systemone","provider":"TypeSafe"},"packing":"one request per paper","requests":1,"input_tokens":4604,"cost_usd_reported":0.000193},"compiled_at":"2026-09-23","bank_version":"abstract-p1-20260923","model_version":"classifier-1.13-20260917","abstract_states":{"claims_first":0.03,"states_limitation":0.3,"human_participants":0.01,"controlled_comparison":0.08,"randomized_assignment":0.01,"states_quantitative_result":0.93,"compares_with_prior_results":0.51,"mentions_code_or_data_availability":0.02},"evidential_basis":{"p":0.96,"value":"simulation or computation","probabilities":{"argument":0.0,"literature":0.0,"proof_or_derivation":0.0,"analysis_of_existing_data":0.04,"observation_or_experiment":0.0,"simulation_or_computation":0.96}},"contribution_type":{"p":0.62,"value":"simulation study","probabilities":{"review":0.0,"method_or_tool":0.0,"empirical_study":0.0,"simulation_study":0.62,"theoretical_result":0.38,"dataset_or_benchmark":0.0,"position_or_commentary":0.0}},"contribution_statement":{"p":0.75,"text":"We discuss radial pulsations excited in evolutionary models of an initial mass of 40 M_\\odot with solar metallicity of Z=0.014, and compare them to micro-variations in the two Galactic LBVs, HR Car and HD 160529.","location":"abstract s3"}},"coverage":{"tier":"abstract","levels_run":["P abstract"],"not_examined":["full text","figures and tables","references and citing sentences","relations to other papers"],"sources_read":["arXiv listing abstract v1"],"levels_not_run":["S sections","T body sentences","C citations","R cross-paper relations"],"sentences_examined":5,"sentences_in_abstract":5},"measured_accuracy":{"url":"https://pith.science/accuracy","measured_on":"2026-10-02","method":"two independent model families labelled a fresh random sample blind; 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