Abstract
We present numerical results from a parameter study of the standing accretion shock instability (SASI), investigating the impact of general relativity (GR) on the dynamics. Using GR hydrodynamics with GR gravity, and nonrelativistic (NR) hydrodynamics with Newtonian gravity, in an idealized model setting, we vary the initial radius of the shock, and by varying its mass and radius in concert, the proto-neutron star compactness. We investigate four compactnesses expected in a post-bounce core-collapse supernova (CCSN). We find that GR leads to a longer SASI oscillation period, with ratios between the GR and NR cases as large as 1.29 for the highest-compactness suite. We also find that GR leads to a slower SASI growth rate, with ratios between the GR and NR cases as low as 0.47 for the highest-compactness suite. We discuss implications of our results for CCSN simulations.
| Original language | English |
|---|---|
| Article number | 38 |
| Journal | Astrophysical Journal |
| Volume | 964 |
| Issue number | 1 |
| DOIs | |
| State | Published - Mar 1 2024 |
Funding
S.J.D., E.E., and A.M. acknowledge support from the National Science Foundation's Gravitational Physics Program under grant NSF PHY 1806692, and E.E., A.M., and J.B. acknowledge support from the National Science Foundation's Gravitational Physics Program under grant 2110177. This research was supported in part by the Exascale Computing Project (17-SC-20-SC), a collaborative effort of the U.S. Department of Energy Office of Science and the National Nuclear Security Administration. This work was conducted in part using the resources of the Advanced Computing Center for Research and Education at Vanderbilt University, Nashville, TN.
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