Ultra-heavy cosmic-ray science: Are r-process nuclei in the cosmic rays produced in supernovae or binary neutron star mergers?
by Walter Binns, M.H. Israel, B.F. Rauch, A.C. Cummings, A.J. Davis, A.W. Labrador, R.A. Leske, R.A Mewaldt, E.C. Stone, M.E. Wiedenbeck, T.J. Brandt, E.R. Christian, J.T. Link, J.W. Mitchell, G.A. de Nolfo, T.T. von Rosenvinge, K. Sakai, M. Sasaki, C.J. Waddington, H.T. Janka, A.L. Melott, G.M. Mason, E-S. Seo, J.H. Adams, F-K. Thielemann, A. Heger, M. Lugaro, and A.J. Westphal
Published onMay 31, 2019
Ultra-heavy cosmic-ray science: Are r-process nuclei in the cosmic rays produced in supernovae or binary neutron star mergers?
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Abstract
Galactic cosmic rays play an important role in the dynamics of matter and magnetic fields in the interstellar medium, and probably also in star formation. There is an opportunity during the coming decade to answer these questions by measuring the relative abundances of every individual element heavier than iron, including the actinides.
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