An artificial, additional viscosity was added to enhance the transport of angular momentum in order to reduce the core rotation rates to be in agreement with asteroseismology observations. We calculated new 2 M ⊙, Z = 0.01 models, rotating at 0, 125, and 250 km s −1 at the start of main sequence. We investigate the s-process during the AGB phase of stellar models whose cores are enforced to rotate at rates consistent with asteroseismology observations of their progenitors and successors. des Maillettes, 1290 Sauverny, SwitzerlandĪims. Observatoire de Genève, Université de Genève, 51 Ch. Milne Centre for Astrophysics, Department of Physics and Mathematics, University of Hull, Hull HU6 7RX, UK JINA-CEE, Michigan State University, East Lansing, MI 48823, USAĮ. School of Physics and Astronomy, University of Edinburgh, Edinburgh EH9 3FD, UKĭepartment of Physics and Astronomy, University of Victoria, Victoria, BC V8P5C2, Canada Monash Centre for Astrophysics (MoCA), School of Physics and Astronomy, Monash University, Victoria 3800, Australia Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo, 5-1-5 Kashiwanoha, 277-8583 Kashiwa, Japan Konkoly Observatory, MTA CSFK, Konkoly Thege Miklós út 15-17, 1121 Budapest, HungaryĮ-mail: Group, Lennard-Jones Laboratories, Keele University, Keele ST5 5BG, UK Astronomical objects: linking to databases.Including author names using non-Roman alphabets.
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