A study of the Heliocentric dependence of Shock Standoff Distance and Geometry using 2.5D MHD Simulations of CME-driven shocks

TL;DR

This study uses 2.5D MHD simulations to analyze how the shock standoff distance relative to CME size varies with heliocentric distance, revealing a linear increase in the proportionality constant and implications for CME structure and magnetic field estimation.

Contribution

It introduces a heliocentric distance-dependent model for the shock standoff distance to CME size ratio, improving understanding of CME geometry and shock dynamics.

Findings

The proportionality constant kdr varies linearly with heliocentric distance.

kdr is approximately 0.8 at distances less than 30Rs.

kdr reaches about 1.8 at 215Rs, indicating more oblate CME structures.

Abstract

We perform four numerical magnetohydrodynamic simulations in 2.5 dimensions (2.5D) of fast Coronal Mass Ejections (CMEs) and their associated shock fronts between 10Rs and 300Rs. We investigate the relative change in the shock standoff distance, Sd, as a fraction of the CME radial half-width, Dob (i.e. Sd/Dob). Previous hydrodynamic studies have related the shock standoff distance for Earths magnetosphere to the density compression ratio (DR,Ru/Rd) measured across the bow shock (Spreiter, Summers and Alksne 1966). The DR coefficient, kdr, which is the proportionality constant between the relative standoff distance (Sd/Dob) and the compression ratio, was semi-empirically estimated as 1.1. For CMEs, we show that this value varies linearly as a function of heliocentric distance and changes significantly for different radii of curvature of the CMEs leading edge. We find that a value of 0.8+-0.1 is more appropriate for small heliocentric distances (<30Rs) which corresponds to the spherical geometry of a magnetosphere presented by Seiff (1962). As the CME propagates its cross section becomes more oblate and the kdr value increases linearly with heliocentric distance, such that kdr= 1.1 is most appropriate at a heliocentric distance of about 80Rs. For terrestrial distances (215Rs) we estimate kdr= 1.8+-0.3, which also indicates that the CME cross-sectional structure is generally more oblate than that of Earths magnetosphere. These alterations to the proportionality coefficients may serve to improve investigations into the estimates of the magnetic field in the corona upstream of a CME as well as the aspect ratio of CMEs as measured in situ.