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High-resolution Three-dimensional Simulations of Core-collapse Supernovae in Multiple Progenitors

  • Authors: Sean M. Couch and Evan P. O'Connor

Couch & O'Connor 2014 The Astrophysical Journal 785 123.

  • Provider: AAS Journals

Caption: Figure 9.

Square root of the powers, , in the first four spherical harmonics of the shock surface, weighted by the mean shock radius, as functions of time, for s15 (left) and s27 (right). Late-time SASI activity in s15 f heat1.00 3D is apparent, as is the early ( t pb < 300 ms) SASI activity in both s27 f heat1.00 3D and s27 f heat 1.05 3D. Notably, there is not so great a difference in the P values between 2D and 3D as reported in some previous 2D vs. 3D studies (Burrows et al. 2012; Couch 2013a).

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