{"paper":{"title":"On the nature of massive helium star winds and Wolf-Rayet-type mass loss","arxiv_id":"2009.01849","primary_cat":"astro-ph.SR","submitted_at":"2020-09-03T18:00:02+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. 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objects.","hedge":{"p":0.98,"label":"asserted"},"own_p":0.05,"main_claim_p":0.06,"quantitative":false,"quantitative_p":0.04,"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":2,"p":0.77,"id":"s2","own":false,"role":"gap","text":"While empirical mass-loss constraints for massive helium stars have improved over the last decades, the resulting recipes are limited to metallicities with the observational ability to sufficiently resolve individual stars.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.05,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.1,"role_probabilities":{"gap":0.77,"method":0.0,"result":0.0,"background":0.2,"limitation":0.03,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":3,"p":0.53,"id":"s3","own":false,"role":"gap","text":"Yet, theoretical efforts have been hampered by the complexity of Wolf-Rayet (WR) winds arising from the more massive helium stars.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.05,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.53,"method":0.0,"result":0.0,"background":0.46,"limitation":0.01,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":4,"p":0.56,"id":"s4","own":true,"role":"method","text":"In an unprecedented effort, we calculate next-generation stellar atmosphere models resembling massive helium main sequence stars with Fe-bump driven winds up to $500\\,M_\\odot$ over a wide metallicity range between $2.0$ and $0.02\\,Z_\\odot$.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.97,"main_claim_p":0.06,"quantitative":true,"quantitative_p":0.98,"role_probabilities":{"gap":0.0,"method":0.56,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.44,"interpretation":0.0}},{"i":5,"p":1.0,"id":"s5","own":true,"role":"result","text":"We uncover a complex $\\Gamma_\\text{e}$-dependency of WR-type winds and their metallicity-dependent breakdown.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.96,"main_claim_p":0.3,"quantitative":false,"quantitative_p":0.05,"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":0.94,"id":"s6","own":true,"role":"interpretation","text":"The latter can be related to the onset of multiple scattering, requiring higher $L/M$-ratios at lower metallicity.","hedge":{"p":0.77,"label":"asserted"},"own_p":0.77,"main_claim_p":0.08,"quantitative":false,"quantitative_p":0.13,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.06,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.94}},{"i":7,"p":0.69,"id":"s7","own":true,"role":"contribution","text":"Based on our findings, we derive the first ever theoretically-motivated mass-loss recipe for massive helium stars.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.97,"main_claim_p":0.6,"quantitative":false,"quantitative_p":0.11,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.31,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.69,"interpretation":0.0}},{"i":8,"p":0.96,"id":"s8","own":true,"role":"result","text":"We also provide estimates for LyC and He II ionizing fluxes, finding stripped helium stars to contribute considerably at low metallicity.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.97,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.21,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.96,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.04,"interpretation":0.0}},{"i":9,"p":0.98,"id":"s9","own":true,"role":"result","text":"In sharp contrast to OB-star winds, the mass loss for helium stars scales with the terminal 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