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This paper presents a study of a large sample of global disturbances in thesolar corona with characteristic propagating fronts as intensity enhancement,similar to the phenomena that have often been referred to as EIT waves or EUVwaves. Now Extreme Ultraviolet (EUV) images obtained by the {\it AtmosphericImaging Assembly} (AIA) on board the {\it Solar Dynamics Observatory} (SDO)provide a significantly improved view of these large-scale coronal propagatingfronts (LCPFs). Between April 2010 and January 2013, a total of 171 LCPFs havebeen identified through visual inspection of AIA images in the 193 \AA\channel. Here we focus on the 138 LCPFs that are seen to propagate across thesolar disk, first studying how they are associated with flares, coronal massejections (CMEs) and type II radio bursts. We measure the speed of the LCPF invarious directions until it is clearly altered by active regions or coronalholes. The highest speed is extracted for each LCPF. It is often considerablyhigher than EIT waves. We do not find a pattern where faster LCPFs decelerateand slow LCPFs accelerate. Furthermore, the speeds are not strongly correlatedwith the flare intensity or CME magnitude, nor do they show an association withtype II bursts. We do not find a good correlation either between the speeds ofLCPFs and CMEs in a subset of 86 LCPFs observed by one or both of the {\itSolar and Terrestrial Relations Observatory} (STEREO) spacecraft as limbevents.

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Large-scale Coronal Propagating Fronts in Solar Eruptions as Observed by  the Atmospheric Imaging Assembly on Board the Solar Dynamics  Observatory\,--\,An Ensemble Study