Search

Image Details

View Article Bookmark & Share

Choose export citation format:

Export Citation
Large resolution
Hi-Resolution Export to PDF

Dependence on the Equation of State in SPH Simulations of Proto-Uranian Disk Formation from a Giant Impact

  • Authors: Keiya Murashima, Takanori Sasaki

Keiya Murashima and Takanori Sasaki 2026 The Astrophysical Journal 1005 .

  • Provider: AAS Journals

Caption: Figure 13.

Initial density profiles of the target (left column) and the impactor (right column) utilizing the SSPH. From top to bottom, the panels show the profiles generated by the SESAME/ANEOS, Tillotson, and HM80 equations of state (EOSs). The radial distance is calculated from the center of mass of each respective body at t = 0.

Other Images in This Article
Image in this article
Image in this article
Image in this article
Image in this article
Image in this article
Image in this article
Image in this article
Image in this article
Image in this article

Show More

Copyright and Terms & Conditions

Additional terms of reuse