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

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.

arXiv comment12 pages, 5 figures, accepted for publication in The Astrophysical Journal

References in corpus (31)

• Thermal Diagnostics with the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory: A Validated Method for Differential Emission Measure Inversions
• The formation of the Halpha line in the solar chromosphere
• Differential Emission Measure Analysis of Multiple Structural Components of Coronal Mass Ejections in the Inner Corona
• The Kinematics of a Globally Propagating Disturbance in the Solar Corona
• 'EUV Waves' are Waves: First Quadrature Observations of an EUV Wave from STEREO
• Magnetohydrodynamic Modeling of the Solar Eruption on 2010 April 8
• First Simultaneous Observation of H-alpha Moreton Wave, EUV Wave, and Filament/Prominence Oscillations
• Large-scale Coronal Propagating Fronts in Solar Eruptions as Observed by the Atmospheric Imaging Assembly on Board the Solar Dynamics Observatory\,--\,An Ensemble Study
• Are "EIT Waves" Fast-Mode MHD Waves?
• Genesis and impulsive evolution of the 2017 September 10 coronal mass ejection
• The Genesis of an Impulsive Coronal Mass Ejection observed at Ultra-High Cadence by AIA on SDO
• Multi-thermal dynamics and energetics of a coronal mass ejection in the low solar atmosphere
• Numerical Experiments of Wave-Like Phenomena Caused by the Disruption of an Unstable Magnetic Configuration
• The Atmospheric Response to High Nonthermal Electron Beam Fluxes in Solar Flares I: Modeling the Brightest NUV Footpoints in the X1 Solar Flare of 2014 March 29
• Understanding the Physical Nature of Coronal "EIT Waves"
• Origins of Rolling, Twisting and Non-Radial Propagation of Eruptive Solar Events
• Interaction of a Moreton/EIT wave and a coronal hole
• Testing magnetofrictional extrapolation with the Titov-Démoulin model of solar active regions
• The fast filament eruption leading to the X-flare on March 29, 2014
• Analysis of a global Moreton wave observed on October 28, 2003
• Analytic modeling of the Moreton wave kinematics
• Coronal response to an EUV wave from DEM analysis
• Improved methods for determining the kinematics of coronal mass ejections and coronal waves
• Case Study of Four Homologous Large-Scale Coronal Waves Observed on 2010 April 28 and 29
• Observations and Modelling of the Pre-Flare Period of the 29 March 2014 X1 Flare
• CorPITA: An Automated Algorithm for the Identification and Analysis of Coronal "EIT Waves"
• A Statistical Analysis of the Solar Phenomena Associated with Global EUV Waves
• Moreton and EUV Waves Associated with an X1.0 Flare and CME Ejection
• The energetics of a global shock wave in the low solar corona
• The Triggering of the 29-March-2014 Filament Eruption
• Two step chromospheric Moreton wave excitation in a blast-wave scenario. A case study: the December 06, 2006 event

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