Cooling and Instabilities in Colliding Flows

Abstract

Collisional self-interactions occurring in protostellar jets give rise to strong shocks, the structure of which can be affected by radiative cooling within the flow. To study such colliding flows, we use the AstroBEAR AMR code to conduct hydrodynamic simulations in both one and three dimensions with a power law cooling function. The characteristic length and time scales for cooling are temperature dependent and thus may vary as shocked gas cools. When the cooling length decreases sufficiently rapidly the system becomes unstable to the radiative shock instability, which produces oscillations in the position of the shock front; these oscillations can be seen in both the one and three dimensional cases. Our simulations show no evidence of the density clumping characteristic of a thermal instability, even when the cooling function meets the expected criteria. In the three-dimensional case, the nonlinear thin shell instability (NTSI) is found to dominate when the cooling length is sufficiently small. When the flows are subjected to the radiative shock instability, oscillations in the size of the cooling region allow NTSI to occur at larger cooling lengths, though larger cooling lengths delay the onset of NTSI by increasing the oscillation period.

12 pages, 21 figures. Accepted for publication in MNRAS

References in corpus (5)

• Simulating Magnetohydrodynamical Flow with Constrained Transport and Adaptive Mesh Refinement; Algorithms & Tests of the AstroBEAR Code
• Episodic Magnetic Bubbles and Jets: Astrophysical Implications from Laboratory Experiments
• Supersonic turbulence in shock-bound interaction zones I: symmetric settings
• Simulations of the non-linear thin shell instability
• Thermal instability revisited

Cited by in corpus (4)

• Shocks in the warm neutral medium I -- Theoretical model
• Shocks in the warm neutral medium II -- Origin of neutral carbon at high pressure
• Morphology of Shocked Lateral Outflows in Colliding Hydrodynamic Flows
• Shock corrugation to the rescue of the internal shock model in microquasars: The single-scale MHD view