Shock identification and classification in 2D MHD compressible turbulence -- Orszag-Tang vortex

Abstract

Compressible magnetohydrodynamic (MHD) turbulence is a common feature of astrophysical systems such as the solar atmosphere and interstellar medium. Such systems are rife with shock waves that can redistribute and dissipate energy. For an MHD system, three broad categories of shocks exist (slow, fast or intermediate) however the occurrence rates of each shock type is not known for turbulent systems. Here we present a method for detecting and classifying the full range of MHD shocks applied to the Orszag-Tang vortex. Our results show that the system is dominated by fast and slow shocks, with far less frequent intermediate shocks appearing most readily near magnetic reconnection sites. We present a potential mechanism that could lead to the formation of intermediate shocks in MHD systems, and study the coherency and abundances of shocks in compressible MHD turbulence.

Accepted for publication in Experimental Results

References in corpus (2)

• Intermediate shock substructures within a slow-mode shock occurring in partially ionised plasma
• Stability of two-fluid partially-ionised slow-mode shock fronts

Cited by in corpus (4)

• Waves in the lower solar atmosphere: the dawn of next-generation solar telescopes
• Detection of magnetohydrodynamic waves by using machine learning
• On the Relationship between Solar Spicules and Propagating Coronal Disturbances: The Role of Shocks
• Decomposing wave activity in the solar atmosphere: Shocks, jets and swirls in the quiet Sun