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Revisiting Impacts of Nuclear Burning for Reviving Weak Shocks in Neutrino-driven Supernovae

  • Authors: Ko Nakamura, Tomoya Takiwaki, Kei Kotake, and Nobuya Nishimura

Nakamura et al. 2014 The Astrophysical Journal 782 91.

  • Provider: AAS Journals

Caption: Figure 5.

Snapshots of velocity profile (top) and composition distribution (bottom) for model LC15 with ( L ν0, 52, t d ) = (2.2, 2.0) at selected postbounce epochs ( t pb = 150, 250, 350, and 400 ms). Solid and dotted lines in the top of each panel show the velocity profile with or without nuclear burning, respectively. In the bottom part, distributions of representative elements of the burning model are shown. Note that the abundances of neutron (n) and proton (p) are estimated from Shen EOS and the others are calculated from the nuclear network calculation. The nucleon-rich region in the abundance plot is separated by a vertical dashed line.

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