# 3D Hydrodynamic Simulation of Classical Nova Explosions**Team:** 66
**School:** Los Alamos High
**Area of Science:** Astrophysics
**Interim:**
Problem Definition:
This project’s goal is to simulate a classical nova explosion. A 3D model will be developed in three main stages, 1) a stable star, 2) orbiting binary between the stable star and white dwarf, and 3) the explosion of the accreted hydrogen gas on the white dwarf.
Problem Solution:
C and MPI are currently being used to run the program. A full N-Body gravity method is implemented, with MLS (Moving Least Squares) to model internal pressure. Simulations have been running to get a stable star. Once a stable star has been achieved, a binary orbit with a white dwarf will be added to model accretion. An explosion will be modeled once enough hydrogen gas has been accreted.
Progress to Date:
Initially, a gravity star implosion was simulated, then an artificial wall was placed at the core to prevent implosion. Internal pressure was added to the simulation to replace the artificial wall. MPI (Message Passing Interface) has been added to the simulations in order to decrease computational time. OpenCL (Open Computing Language) will be implemented soon for a faster N-Body gravity calculation.
Expected Result:
My simulation should currently give a stable star, which will then be put in a binary orbit around a White Dwarf to begin the nova simulation. After the hydrogen gas accretes on the surface of the White Dwarf, it should explode. At this point, different simulations will be run to compare to experimental and professional results, and also different initial variables (masses, separation, distance and temperature) to determine effects on novae explosions.
References:
1) Dilts A. Gary, “Moving-Least-Squares-Particle Hydrodynamics-I. Consistency and Stability” International Journal for Numerical Methods in Engineering 44, 1115-1155 (1999). Print.
2) Nealen, Andrew. “An As-Short-As-Possible Introduction to the Least Squares, Weighted Least Squares, and Moving Least Squares Methods for Scattered Data Approximation and Interpolation”
3) Brownlee, R., et. al. “Enhancing SPH using Moving Least-Squares and Radial Basis Functions”
4) Braithwaite, Jonathan. “An Introduction to Hydrodynamics and Astrophysical Magnetohydrodynamics.” Mar. 2011.
5) Loren-Aguilar, P., et. al. “Smoothed Particle Hydrodynamics simulations of white dwarf collisions and close encounters.” Royal Astronomical Society: Apr. 2010. Print.
**Team Members:**
Coleman Kendrick
**Sponsoring Teacher:** Brian Kendrick
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