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Ledoux Convection in Protoneutron Stars—A Clue to Supernova Nucleosynthesis?

  • Authors: Wolfgang Keil, H.-Thomas Janka, and Ewald Müller

Keil, Janka, & Müller 1996 The Astrophysical Journal Letters 473 L111.

  • Provider: AAS Journals

Caption: Fig. 3.

(a) and (b) Absolute values of the velocity for the two‐dimensional simulation at times t = 0.525 s and t = 1.047 s, respectively, color‐coded in units of 108 cm s−1. The computation was performed in an angular wedge of 90° between +45° and −45° around the equatorial plane. The PNS has contracted to a radius of about 21 km at the given times. (c) and (d) Relative deviations of the electron fraction Ye from the angular means langYerang at each radius for the same two instants. Maximum deviations are of the order of 30%. Lepton‐rich matter rises while deleptonized material sinks in. Comparison of both times shows that the inner edge of the convective layer moves inward from about 8.5 km at t = 0.525 s to less than 2 km at t = 1.047 s.

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