# Quantifying the relationship between Moreton-Ramsey waves and "EIT waves" using observations of 4 homologous wave events

## TL;DR

This study analyzes four homologous solar global waves observed in EUV and H-alpha, quantifying their kinematics and connection, revealing that EUV waves are faster and weaker shocks than their associated Moreton-Ramsey waves, with magnetic field influence affecting their evolution.

## Contribution

It provides the first joint observations of EUV and Moreton-Ramsey waves for multiple events, quantifying their relationship and proposing a magnetic field influence on wave evolution.

## Key findings

- EUV waves exhibit higher initial velocities than Moreton-Ramsey waves.
- Both wave types are weakly shocked with Mach numbers just above one.
- Global waves are influenced by surrounding magnetic fields, affecting their propagation.

## Abstract

Freely-propagating global waves in the solar atmosphere are commonly observed using Extreme UltraViolet passbands (EUV or "EIT waves"), and less regularly in H-alpha (Moreton-Ramsey waves). Despite decades of research, joint observations of EUV and Moreton-Ramsey waves remain rare, complicating efforts to quantify the connection between these phenomena. We present observations of four homologous global waves originating from the same active region between 28-30 March 2014 and observed using both EUV and H-alpha data. Each global EUV wave was observed by the Solar Dynamics Observatory, with the associated Moreton-Ramsey waves identified using the Global Oscillations Network Group (GONG) network. All of the global waves exhibit high initial velocity (e.g., 842-1388 km s$^{-1}$ in the 193A passband) and strong deceleration (e.g., -1437 - -782 m s$^{-2}$ in the 193A passband) in each of the EUV passbands studied, with the EUV wave kinematics exceeding those of the Moreton-Ramsey wave. The density compression ratio of each global wave was estimated using both differential emission measure and intensity variation techniques, with both indicating that the observed waves were weakly shocked with a fast magnetosonic Mach number slightly greater than one. This suggests that, according to current models, the global coronal waves were not strong enough to produce Moreton-Ramsey waves, indicating an alternative explanation for these observations. Instead, we conclude that the evolution of the global waves was restricted by the surrounding coronal magnetic field, in each case producing a downward-angled wavefront propagating towards the north solar pole which perturbed the chromosphere and was observed as a Moreton-Ramsey wave.