Eric J. Lingerfelt

The development of explosions in axisymmetric ab initio core-collapse supernova simulations of 12–25 M⊙ stars

We present four ab initio axisymmetric core-collapse supernova simulations for 12, 15, 20, and 25

Big, Deep, and Smart Data in Scanning Probe Microscopy

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Near Real-time Data Analysis of Core-Collapse Supernova Simulations With Bellerophon

progenitors. All of the simulations yield explosions and have been evolved for at least 1.2 seconds after core bounce and 1 second after material first becomes unbound. Simulations were computed with our Chimera code employing spectral neutrino transport, special and general relativistic transport effects, and state-of-the-art neutrino interactions. Continuing the evolution beyond 1 second allows explosions to develop more fully and the processes powering the explosions to become more clearly evident. We compute explosion energy estimates, including the binding energy of the stellar envelope outside the shock, of 0.34, 0.88, 0.38, and 0.70 B (

BEAM: A Computational Workflow System for Managing and Modeling Material Characterization Data in HPC Environments

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A Multitier System for the Verification, Visualization and Management of CHIMERA

ergs) and increasing at 0.03, 0.15, 0.19, and 0.52 B s

Bottlenecks and Waiting Points in Nucleosynthesis in X‐ray bursts and Novae

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Waiting Points in Nova and X‐ray burst Nucleosynthesis

, respectively, for the 12, 15, 20, and 25

Computational Infrastructure for Nuclear Astrophysics

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Distributed workflows for modeling experimental data

models. Three models developed pronounced prolate shock morphologies, while the 20

High Performance Computing Tools for Cross Correlation of Multi-Dimensional Data Sets Across Instrument Platforms

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