Sean M. Couch1,2,3,4 Kristen Dage1 Erika Lustig1 1 Department of Physics and Astronomy, Michigan State University 2 Department of Computational Mathematics, Science, and Engineering, Michigan State University 3 National Superconducting Cyclotron Laboratory, Michigan State University 4 Joint Institute for Nuclear Astrophysics, Michigan State University

Abstracthooray!

Introduction

This is new!

Colella and Glaz (1985)11This is a test

Numerical Experiments

• Could try not tracing the $$\gamma_{e}$$. First order in time approach.

• Zingale & Katz with UHD. Both with Helmholtz and Nuclear. But Nuclear doesn’t go down so low…

• do Helmholtz at high density/temperature in range of Nuclear. Will need to determine the appropriate $$\sum Y_{i}$$. Might be able to determine this from data in the table. If $$\bar{A}$$ and $$\bar{Z}$$ are available…

• Should also try ”EOSforRiemann” approach.

• Need to address construction of wave speeds in HLLC for general EOS (Zingale and Katz, 2015)

References

1. Phillip Colella, Harland M Glaz. Efficient solution algorithms for the Riemann problem for real gases. Journal of Computational Physics 59, 264–289 Elsevier BV, 1985. Link

2. Phillip Colella, Paul R Woodward. The Piecewise Parabolic Method (PPM) for gas-dynamical simulations. Journal of Computational Physics 54, 174–201 Elsevier BV, 1984. Link

3. Michael Zingale, Max P. Katz. ON THE PIECEWISE PARABOLIC METHOD FOR COMPRESSIBLE FLOW WITH STELLAR EQUATIONS OF STATE. ApJS 216, 31 IOP Publishing, 2015. Link