On physical and numerical instabilities arising in simulations of non-stationary radiatively cooling shocks

Abstract

We describe our modelling of the radiatively cooling shocks and their thin shells with various numerical tools in different physical and calculational setups. We inspect structure of the dense shell, its formation and evolution, pointing out physical and numerical factors that sustain its shape and also may lead to instabilities. We have found that under certain physical conditions, the circular shaped shells show a strong bending instability and successive fragmentation on Cartesian grids soon after their formation, while remain almost unperturbed when simulated on polar meshes. We explain this by physical Rayleigh--Taylor like instabilities triggered by corrugation of the dense shell surfaces by numerical noise. Conditions for these instabilities follow from both the shell structure itself and from episodes of transient acceleration during re-establishing of dynamical pressure balance after sudden radiative cooling onset. They are also easily excited by physical perturbations of the ambient medium. The widely mentioned Non-linear Thin Shell Instability, in contrast, in tests with physical perturbations is shown to have only limited chances to develop in real radiative shocks, as it seems to require a special spatial arrangement of fluctuations to be excited efficiently. The described phenomena also set new requirements on further simulations of the radiatively cooling shocks in order to be physically correct and free of numerical artefacts.

arXiv comment25 pages, 14 figures, accepted for publication in MNRAS, several references updated and the spelling is fixed to match the journal version

References in corpus (22)

• PLUTO: a Numerical Code for Computational Astrophysics
• The Physics of Gamma-Ray Bursts and Relativistic Jets
• Supernova remnants: the X-ray perspective
• Momentum Injection by Supernovae in the Interstellar Medium
• Nonlinear Instabilities in Shock-Bounded Slabs
• Supernova Feedback in an Inhomogeneous Interstellar Medium
• Supernova Remnants in Molecular Clouds
• A new radiative cooling curve based on an up to date plasma emission code
• Diffusive Shock Acceleration with Magnetic Amplification by Non-resonant Streaming Instability in SNRs
• Enhanced Momentum Feedback from Clustered Supernovae
• An Exact Integration Scheme for Radiative Cooling in Hydrodynamical Simulations
• Numerical models of collisions between core-collapse supernovae and circumstellar shells
• Cosmic ray driven Galactic winds
• Supernova Remnants Interacting with Molecular Clouds: X-ray and Gamma-ray Signatures
• Simulating radiative astrophysical flows with the PLUTO code: A non-equilibrium, multi-species cooling function
• Numerical overcooling in shocks
• Dynamics of a Supernova Envelope in a Cloudy Interstellar Medium
• Magnetic field amplification by collisionless shocks in partially ionized plasmas
• Post-adiabatic supernova remnants in the interstellar magnetic field. Parallel and perpendicular shocks
• Simulations of the non-linear thin shell instability
• Study of Supernovae Important for Cosmology
• Spectra of accelerated particles at supernova shocks in the presence of neutral hydrogen: the case of Tycho

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