Evolution of the Alfvén Mach number associated with a coronal mass ejection shock

Abstract

The Sun regularly produces large-scale eruptive events, such as coronal mass ejections (CMEs) that can drive shock waves through the solar corona. Such shocks can result in electron acceleration and subsequent radio emission in the form of a type II radio burst. However, the early-phase evolution of shock properties and its relationship to type II burst evolution is still subject to investigation. Here we study the evolution of a CME-driven shock by comparing three commonly used methods of calculating the Alfvén Mach number ($M_A$), namely: shock geometry, a comparison of CME speed to a model of the coronal Alfvén speed, and the type II band-splitting method. We applied the three methods to the 2017 September 2 event, focusing on the shock wave observed in extreme ultraviolet (EUV) by the Solar Ultraviolet Imager (SUVI) on board GOES-16, in white-light by the Large Angle and Spectrometric Coronagraph (LASCO) on board SOHO, and the type II radio burst observed by the Irish Low Frequency Array (I-LOFAR). We show that the three different methods of estimating shock $M_A$ yield consistent results and provide a means of relating shock property evolution to the type II emission duration. The type II radio emission emerged from near the nose of the CME when $M_A$ was in the range 1.4-2.4 at a heliocentric distance of $\sim$1.6 $R_{\odot }$. The emission ceased when the CME nose reached $\sim$2.4 $R_{\odot }$, despite an increasing Alfvén Mach number (up to 4). We suggest the radio emission cessation is due to the lack of quasi-perpendicular geometry at this altitude, which inhibits efficient electron acceleration and subsequent radio emission.

8 pages, 4 figures

References in corpus (8)

• The formation heights of coronal shocks from 2D density and Alfvén speed maps
• Off-limb Solar Coronal Wavefronts From SDO/AIA EUV Observations - Implications For Particle Production
• Observations of an Eruptive Solar Flare in the Extended EUV Solar Corona
• Quasiperiodic acceleration of electrons by a plasmoid-driven shock in the solar atmosphere
• Three-dimensional reconstruction of CME-driven shock-streamer interaction from radio and EUV observations: a different take on the diagnostics of coronal magnetic fields
• Understanding CME and associated shock in the solar corona by merging multi wavelengths observation
• Properties of a Coronal Shock Wave as A Driver of Early SEP Acceleration
• A Decade of Coronagraphic and Spectroscopic Studies of CME-Driven Shocks

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