Very massive close binaries and the puzzling temporal evolution of 14N in the Solar Neighbourhood |
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| Affiliation: | 1. Department of Physics and Astronomy, Arizona State University, Tempe, Arizona 85287-1504, USA;2. Department of Astronomy and Astrophysics, Enrico Fermi Institute, University of Chicago, 933 E. 56th St, Chicago, IL 60637, USA;3. XNH, Nuclear and Hydrodynamic Applications, MS F664, Los Alamos National Laboratory, Los Alamos, NM 87545, USA;1. W.M. Keck Science Center, Science Department, Scripps College, Claremont Colleges, 925 North Mills Avenue, Claremont, CA 91711, USA;2. Center for Astrophysics and Space Sciences, University of California San Diego, La Jolla, CA 92093, USA;1. INAF Astronomical Observatory of Padova, 36012 Asiago (VI), Italy;2. ANS Collaboration, c/o Osservatorio Astronomico, via dell’Osservatorio 8, 36012 Asiago (VI), Italy;1. Department of Physics, University of Basel, Switzerland;2. Department of Physics, NC State University, USA;3. GSI Darmstadt, Germany;4. Max Planck Institute for Chemistry, Mainz, Germany;5. Institute for Theoretical & Experimental Physics, Moscow, Russia;1. Laboratory for Space Sciences and Physics Department, Washington University, St. Louis, MO 63130, USA;2. Naval Research Laboratory, Washington, DC 20375, USA;3. University of Missouri, Columbia, MO 65211, USA |
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| Abstract: | Low metallicity very massive stars with an initial mass between 140M⊙ and 260M⊙ can be subdivided into two groups: those between 140M⊙ and 200M⊙ which produce a relatively small amount of Fe, and those with a mass between 200M⊙ and 260M⊙ where the Fe-yield ejected during the supernova explosion is enormous. We first demonstrate that the inclusion of the second group into a chemical evolutionary model for the Solar Neighbourhood predicts an early temporal evolution of Fe, which is at variance with observations whereas it cannot be excluded that the first group could have been present. We then show that a low metallicity binary with very massive components (with a mass corresponding to the first group) can be an efficient site of primary 14N production through the explosion of a binary component that has been polluted by the pair instability supernova ejecta of its companion. When we implement these massive binary 14N yields in a chemical evolution model, we conclude that very massive close binaries may be important sites of 14N enrichment during the early evolution of the Galaxy. |
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