Computational fluid dynamics simulations using the WENO method and level set method are applied to high Mach number nonrelativistic astrophysical jets, including the effects of radiative cooling. WENO methods introduced in Liu et al. (J. Comput. Phys., 115:200–212, 1994) have allowed us to simulate HH 1-2 astrophysical jets at Mach number much higher than Mach 80 (Ha et al. in J. Sci. Comput. 2...

We generalize the Raychaudhuri equation for the evolution of a self gravitating fluid to include an Abelian and non-Abelian hybrid magneto fluid at a finite temperature. The aim is to utilize this equation for investigating the dynamics of astrophysical high temperature Abelian and non-Abelian plasmas.

Turbulent reconnection allows fast magnetic reconnection of astrophysical magnetic fields. This entails numerous astrophysical implications and opens new ways to approach long standing problems. I briefly discuss a model of turbulent reconnection within which the stochasticity of 3D magnetic field enables rapid reconnection through both allowing multiple reconnection events to take place simult...

Fini te difference simulation of f l u i d flows under astrophysical conditions is often complicated by factors such as complex gas physics, the occurrence of dynamics at widely d i f fer ing length scales, and the necessity of using imp l i c i t d i f ference equations. This report describes a simple, general, and e f f i c i en t algorithm for solving one-dimensional, spherical ly symmetric ...

The idea of this work is to compare a new positive and entropy stable approximate Riemann solver by Francois Bouchut with a state-of the-art algorithm for astrophysical fluid dynamics. We implemented the new Riemann solver into an astrophysical PPM-code, the Prometheus code, and also made a version with a different, more theoretically grounded higher order algorithm than PPM. We present shock t...

in astrophysics necessarily involves the development of models and simulation technology to help us understand the complex phenomena underlying astrophysical events. As with any modeling approach, numerical models and simulation codes developed for astrophysical applications must be thoroughly verified and validated to demonstrate their accuracy and assess their credibility. Although verificati...

In astrophysical flows, radiation often contains a large fraction of the energy density, momentum density, and stress (i.e., pressure) in the radiating fluid. Furthermore, radiative transfer is usually the most effective energy-exchange mechanism within the fluid. To describe the behavior of such flows we need conservation laws that account accurately for both the material and the radiative con...

A lagrangian for relativistic fluid systems with matters inside is developed using gauge principle. In the model, the gauge boson represents the fluid field in a form Aμ ≡ ǫμ φ, where ǫμ contains the fluid kinematics and φ is an auxiliary field representing the fluid distribution. This leads to a new relativistic equation of motion for fluid, but which further coincides to the classical Euler e...