New s-process Mechanism in Rapidly Rotating Massive Population II Stars

Projjwal Banerjee, Alexander Heger, Yong Zhong Qian

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Abstract

We report a new mechanism for the s-process in rotating massive metal-poor stars. Our models show that above a critical rotation speed, such stars evolve in a quasi-chemically homogeneous fashion, which gives rise to a prolific s-process. Rotation-induced mixing results in primary production of 13C, which subsequently makes neutrons via 13C(α, n)16O during core He burning. Neutron capture can last up to ∼ 1013 (∼3 × 105 yr) with the peak central neutron density ranging from ∼107 to 108 cm-3. Depending on the rotation speed and the mass loss rate, a strong s-process can occur with production of elements up to Bi for progenitors with initial metallicities of [Z] ≲ -1.5. This result suggests that rapidly rotating massive metal-poor stars are likely the first sites of the main s-process. We find that these stars can potentially explain the early onset of the s-process and some of the carbon-enhanced metal-poor (CEMP-s and CEMP-r/s) stars with strong enrichment attributed to the s-process or a mixture of the r-process and the s-process.

Original languageEnglish (US)
Article number187
JournalAstrophysical Journal
Volume887
Issue number2
DOIs
StatePublished - Dec 20 2019

Bibliographical note

Funding Information:
Projjwal Banerjee Alexander Heger Yong-Zhong Qian Projjwal Banerjee Alexander Heger Yong-Zhong Qian Department of Astronomy, School of Physics and Astronomy, Shanghai Jiao Tong University, Shanghai 200240, People’s Republic of China Department of Physics, Indian Institute of Technology Palakkad, Palakkad, Kerala 678557, India Monash Centre for Astrophysics, School of Physics and Astronomy, Monash University, Vic 3800, Australia Tsung-Dao Lee Institute, Shanghai 200240, People's Republic of China School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA Projjwal Banerjee, Alexander Heger and Yong-Zhong Qian 2019-12-20 2019-12-18 14:12:26 cgi/release: Article released bin/incoming: New from .zip National Natural Science Foundation of China 11533006 11655002 US Department of Energy DE-FG02-87ER40328 Science and Technology Commission of Shanghai Municipality 16DZ2260200 yes We report a new mechanism for the s -process in rotating massive metal-poor stars. Our models show that above a critical rotation speed, such stars evolve in a quasi-chemically homogeneous fashion, which gives rise to a prolific s -process. Rotation-induced mixing results in primary production of 13 C, which subsequently makes neutrons via during core He burning. Neutron capture can last up to (∼3 � 10 5 yr) with the peak central neutron density ranging from ∼10 7 to 10 8 . Depending on the rotation speed and the mass loss rate, a strong s -process can occur with production of elements up to Bi for progenitors with initial metallicities of [ Z ]�≲�−1.5. This result suggests that rapidly rotating massive metal-poor stars are likely the first sites of the main s -process. We find that these stars can potentially explain the early onset of the s -process and some of the carbon-enhanced metal-poor (CEMP- s and CEMP- r/s ) stars with strong enrichment attributed to the s -process or a mixture of the r -process and the s -process. � 2019. 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