Type III Metric Radio-Wave Activity Prior to and During Active Region Flaring and CMEs (Invited)

Details Type III Metric Radio-Wave Activity Prior to and During Active Region Flaring and CMEs (Invited) Type III Metric Radio-Wave Activity Prior to and During Active Region Flaring and CMEs (Invited)

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh54d..03j&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH54D-03

Astronomy and Astrophysics

Astrophysics

[6954] Radio Science / Radio Astronomy, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7519] Solar Physics, Astrophysics, And Astronomy / Flares, [7534] Solar Physics, Astrophysics, And Astronomy / Radio Emissions

Scientific paper

From the time that type III metric radio-wave activity has been known, and imaged, there has been a realization that this activity often increases during, and for some events from a few minutes to several hours prior to the major manifestations observed for a flare or Coronal Mass Ejection (CME). We review these analyses from as long ago as the observations from Culgoora, Australia, and more recently from the French Nancay radio observatory. We find there can be precursor activity before a flare or CME as indicated by the increasing numbers of isolated type III bursts, and that this can be a maximum prior to the most obvious manifestation of either the surface flare or the most obvious rapid outward coronal motion of a CME. Current imaging measurements from the Nancay radio array further clarify the location of this activity for specific events such as the 26 April 2008 CME that was observed just following the Whole Heliosphere Interval (WHI) near the time of solar minimum. A plausible explanation for this precursor activity exists, and we expect that this idea can be more fully tested using present-day observations. As solar activity increases and more observations become available from, for instance, the Murchison Widefield Array (MWA) now under construction in Western Australia, far better worldwide temporal coverage for this type of analysis will exist. In conjunction with current NASA instrumentation such as the Solar TErrestrial RElations Observatory (STEREO) and SOlar and Heliospheric Observatory (SOHO) coronagraphs, and the Solar Dynamics Observatory (SDO), we expect a significant improvement in our understanding of this unique flare and CME precursor activity.

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