{"paper":{"title":"Photometric variability of blue supergiants: Constraints on stellar masses and evolutionary stages","arxiv_id":"2610.28352","primary_cat":"astro-ph.SR","submitted_at":"2026-10-20T15:18:31+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. 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":"Blue supergiants (BSGs) are crucial to understanding the evolution of massive stars.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.03,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.03,"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":0.88,"id":"s1","own":false,"role":"background","text":"Although distinguishing between pre- and post-red supergiant (RSG) phases is challenging, stellar pulsations provide valuable constraints on their masses and evolutionary status.","hedge":{"p":0.97,"label":"asserted"},"own_p":0.05,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.11,"role_probabilities":{"gap":0.12,"method":0.0,"result":0.0,"background":0.88,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":0.72,"id":"s2","own":true,"role":"contribution","text":"This study analyzes TESS light curves of six BSGs with high L/M to identify periodicities.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.95,"main_claim_p":0.02,"quantitative":true,"quantitative_p":0.94,"role_probabilities":{"gap":0.0,"method":0.28,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.72,"interpretation":0.0}},{"i":3,"p":0.97,"id":"s3","own":true,"role":"method","text":"We performed theoretical modeling of the radial unstable modes to characterize the strange modes.","hedge":{"p":0.94,"label":"asserted"},"own_p":0.95,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.03,"role_probabilities":{"gap":0.0,"method":0.97,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.03,"interpretation":0.0}},{"i":4,"p":0.9,"id":"s4","own":false,"role":"contribution","text":"We aim to estimate asteroseismic masses, compare them with spectroscopic and evolutionary mass estimates, and assess the evolutionary stage of the stars.","hedge":{"p":0.47,"label":"unclear"},"own_p":0.42,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.25,"role_probabilities":{"gap":0.0,"method":0.02,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.08,"contribution":0.9,"interpretation":0.0}},{"i":5,"p":1.0,"id":"s5","own":true,"role":"method","text":"We employed the Lomb-Scargle periodogram and the weighted wavelet Z-transform to address quasiperiodic behavior and time-varying signals.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.96,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.06,"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":6,"p":1.0,"id":"s6","own":true,"role":"method","text":"A linear nonadiabatic stability analysis was performed to test for radial perturbations, generating eigenfrequencies that enable stellar mass estimation.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.03,"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":7,"p":0.54,"id":"s7","own":true,"role":"contribution","text":"In addition, we characterized the stochastic low-frequency variability (SLFV).","hedge":{"p":0.93,"label":"asserted"},"own_p":0.95,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.03,"role_probabilities":{"gap":0.0,"method":0.44,"result":0.02,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.54,"interpretation":0.0}},{"i":8,"p":0.77,"id":"s8","own":true,"role":"result","text":"We derive a first guess at the asteroseismic masses.","hedge":{"p":0.68,"label":"asserted"},"own_p":0.97,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.02,"result":0.77,"background":0.0,"limitation":0.02,"future_work":0.0,"contribution":0.19,"interpretation":0.0}},{"i":9,"p":0.96,"id":"s9","own":true,"role":"result","text":"We find that HD 74371 and HD 79186 are evolving blueward following the RSG phase, while the evolutionary stage of HD 115842 cannot be uniquely determined with the available mass estimates.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.97,"main_claim_p":0.22,"quantitative":false,"quantitative_p":0.25,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.96,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.04}},{"i":10,"p":0.97,"id":"s10","own":true,"role":"result","text":"We also find that HD 52382 and HD 99953 are likely in the post-RSG phase; however, their low masses are difficult to reconcile with the available evolutionary models.","hedge":{"p":0.99,"label":"hedged_possibility"},"own_p":0.96,"main_claim_p":0.08,"quantitative":false,"quantitative_p":0.23,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.97,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.03}},{"i":11,"p":0.78,"id":"s11","own":true,"role":"result","text":"The extreme supergiant HD 80077 shows the largest mass discrepancy in the sample, suggesting a more complex evolutionary history.","hedge":{"p":0.92,"label":"hedged_possibility"},"own_p":0.92,"main_claim_p":0.07,"quantitative":true,"quantitative_p":0.76,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.78,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.22}},{"i":12,"p":0.93,"id":"s12","own":true,"role":"result","text":"The SLFV properties do not provide a clear diagnostic of the evolutionary stage.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.91,"main_claim_p":0.08,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.93,"background":0.0,"limitation":0.04,"future_work":0.0,"contribution":0.0,"interpretation":0.03}},{"i":13,"p":1.0,"id":"s13","own":true,"role":"interpretation","text":"These results highlight the potential of asteroseismology as a complementary tool for constraining the evolutionary status of BSGs.","hedge":{"p":0.65,"label":"hedged_possibility"},"own_p":0.55,"main_claim_p":0.68,"quantitative":false,"quantitative_p":0.07,"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}},{"i":14,"p":0.79,"id":"s14","own":true,"role":"future_work","text":"However, the mass discrepancies found for some objects indicate that additional observational and theoretical efforts are required.","hedge":{"p":0.59,"label":"hedged_possibility"},"own_p":0.62,"main_claim_p":0.16,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.21,"future_work":0.79,"contribution":0.0,"interpretation":0.0}}]},"compiled":{"main_claim":{"p":0.99,"text":"These results highlight the potential of asteroseismology as a complementary tool for constraining the evolutionary status of BSGs.","location":"abstract s13","hedge_strength":{"p":0.65,"label":"hedged possibility"}},"provenance":{"route":{"via":"TypeSafe API","model":"classifier-1.13.0","endpoint":"https://api.typesafe.ai/v1/systemone","provider":"TypeSafe"},"packing":"one request per paper","requests":1,"input_tokens":10772,"cost_usd_reported":0.0},"compiled_at":"2026-10-21","bank_version":"abstract-p1-20260923","model_version":"classifier-1.13.0","abstract_states":{"claims_first":0.04,"states_limitation":0.97,"human_participants":0.01,"controlled_comparison":0.07,"randomized_assignment":0.01,"states_quantitative_result":0.19,"compares_with_prior_results":0.87,"mentions_code_or_data_availability":0.03},"evidential_basis":{"p":0.9,"value":"analysis of existing data","probabilities":{"argument":0.0,"literature":0.0,"proof_or_derivation":0.0,"analysis_of_existing_data":0.9,"observation_or_experiment":0.09,"simulation_or_computation":0.01}},"contribution_type":{"p":0.99,"value":"empirical study","probabilities":{"review":0.0,"method_or_tool":0.0,"empirical_study":0.99,"simulation_study":0.01,"theoretical_result":0.0,"dataset_or_benchmark":0.0,"position_or_commentary":0.0}},"contribution_statement":{"p":0.86,"text":"This study analyzes TESS light curves of six BSGs with high L/M to identify periodicities.","location":"abstract s2"}},"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":15,"sentences_in_abstract":15},"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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