Seismic Data Preparation Procedures

Schmidt, Andrey; Wilson, Kimberly S

doi:10.21236/ada049922

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1985

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“…(13a)) inducing a drastic change of the predicted element distribution. However for a quantitative analysis [32] the emission of fast e-particles should be taken into account which contribute considerably to an asymmetric element distribution in Ne-induced reactions [33].…”

Section: Discussionmentioning

confidence: 99%

Mass transport and energy equilibration in heavy ion collisions

Schmidt

1985

Z Physik A

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The lack of mass drift observed in Kr-induced collisions is explained assuming energy and particle transfer from the light to the heavy fragment during the equilibration stage in asymmetric heavy-ion reactions. Transferred energy and particle number can be estimated from the interfragment thermal equilibrium distribution provided the initial partition is known which we calculate within a semiclassical theory based on TDHF. The experimental findings are consistent with the theoretical predictions. In particular, the experimental mass drift as function of total kinetic energy loss is quantitatively described within a modified diffusion model which takes into account the mass exchange prior to the transport stage.

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Section: Discussionmentioning

confidence: 99%

Mass transport and energy equilibration in heavy ion collisions

Schmidt

1985

Z Physik A

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“…This figure shows profiles of the central cluster at z = 0 in a simulation using nested initial conditions. The data is taken from [87] and the cluster halo corresponds to halo 1 in [92]. The upper panel shows the overdensity δ, the central one the temperature T and the lower one the turbulent Mach number…”

Section: Cluster Simulationsmentioning

confidence: 99%

Modelling turbulent effects of stellar feedback in cosmological simulations

Frederik¹

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Seismic Data Preparation Procedures

Cited by 2 publications

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Mass transport and energy equilibration in heavy ion collisions

Mass transport and energy equilibration in heavy ion collisions

Modelling turbulent effects of stellar feedback in cosmological simulations

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