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Growing Planets Produce Extreme Dust Signatures

  • Authors: Philip J. Carter, Zoë M. Leinhardt

Philip J. Carter and Zoë M. Leinhardt 2026 The Astrophysical Journal Letters 1007 .

  • Provider: AAS Journals

Caption: Figure 2.

The mass of vaporized ejecta scales with the modified kinetic energy of the collision. Mass of vaporized ejecta, Mvapejecta, as a function of modified kinetic energy, ﹩{K}_{{\rm{R}}}^{{\prime} }﹩. The shape of symbols corresponds to the mass ratio of the collision and the color corresponds to the impact parameter, b. The solid black line and gray band indicate the best-fitting power law and the range of fits obtained via bootstrap fitting. The amplitude is ﹩1.2{2}_{-0.65}^{+1.39}\times 1{0}^{-6}﹩ and the power-law index is 1.01 ± 0.01. The full fit parameters are provided in Table H1. Note the “uncertainties” (derived from the final 10 hr of simulation time, see Section 2.2) are too small to be seen for the majority of collisions.

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