Large-scale Coronal Propagating Fronts During the Rising Phase of Solar Cycle 24

Details Large-scale Coronal Propagating Fronts During the Rising Phase of Solar Cycle 24 Large-scale Coronal Propagating Fronts During the Rising Phase of Solar Cycle 24

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh23a1941n&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH23A-1941

Astronomy and Astrophysics

Astrophysics

[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7514] Solar Physics, Astrophysics, And Astronomy / Energetic Particles, [7519] Solar Physics, Astrophysics, And Astronomy / Flares, [7549] Solar Physics, Astrophysics, And Astronomy / Ultraviolet Emissions

Scientific paper

With increasing solar activity, the AIA on SDO has observed a number of large-scale coronal propagating fronts, which are often called "EIT waves." Although their nature is still actively debated, these propagating fronts usually accompany CMEs, and, in certain cases, may signify CME-related shock waves important for particle acceleration. Using the unprecedented temporal resolution and broad temperature coverage of the AIA, it is possible to characterize the propagating fronts in the corona far better than before, as demonstrated in the literature for a yet small number of cases. We study the properties of more than 40 propagating fronts as observed by AIA, and discuss the key properties for them to be associated with other phenomena such as type II radio bursts, flares, CMEs, ICMEs, and SEP events. We make use of data, both remote-sensing and in-situ, from STEREO which provides two additional vantage points, to make the associations more solid. For the associated phenomena, their basic properties are correlated with those of the propagating fronts. We also revisit the association of EIT waves with other phenomena during the similar phase of Solar Cycle 23 and discuss possible differences in terms of global magnetic field. Understanding their relation with other phenomena, we can have a more complete picture of the coronal propagating fronts in the context of CME acceleration and deceleration.

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