# Effects of Coronal Density and Magnetic Field Distributions on a Global Solar EUV Wave

## TL;DR

This study examines how coronal density and magnetic field variations influence the behavior and propagation of a large-scale EUV wave associated with a CME-driven shock, revealing complex interactions with coronal structures.

## Contribution

It provides new insights into the effects of coronal magnetic and density structures on EUV wave evolution and their connection with CME-driven shocks.

## Key findings

- EUV wave remains connected with the shock after crossing the Sun's far side.
- EUV wave accelerates in low-density, closed magnetic regions.
- Wave interacts with magnetic structures, turning around bright points.

## Abstract

We investigate a global extreme-ultraviolet (EUV) wave associated with a coronal mass ejection (CME)-driven shock on 2017 September 10. The EUV wave is transmitted by north- and south-polar coronal holes (CHs), which is observed by the Solar Dynamics Observatory (SDO) and Solar Terrestrial Relations Observatory A (STEREO-A) from opposite sides of the Sun. We obtain key findings on how the EUV wave interacts with multiple coronal structures, and on its connection with the CME-driven shock: (1) the transmitted EUV wave is still connected with the shock that is incurvated to the Sun, after the shock has reached the opposite side of the eruption; (2) the south CH transmitted EUV wave is accelerated inside an on-disk, low-density region with closed magnetic fields, which implies that an EUV wave can be accelerated in both open and closed magnetic field regions; (3) part of the primary EUV wavefront turns around a bright point (BP) with a bipolar magnetic structure when it approaches a dim, low-density filament channel near the BP; (4) the primary EUV wave is diffused and apparently halted near the boundaries of remote active regions (ARs) that are far from the eruption, and no obvious AR related secondary waves are detected; (5) the EUV wave extends to an unprecedented scale of ~360{\deg} in latitudes, which is attributed to the polar CH transmission. These results provide insights into the effects of coronal density and magnetic field distributions on the evolution of an EUV wave, and into the connection between the EUV wave and the associated CME-driven shock.