Type III Radio Bursts Observed with Radio Spectrograph ARTEMIS IV within the Intense Active Period of October-November 2003

Details Type III Radio Bursts Observed with Radio Spectrograph ARTEMIS IV within the Intense Active Period of October-November 2003 Type III Radio Bursts Observed with Radio Spectrograph ARTEMIS IV within the Intense Active Period of October-November 2003

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1203..133t&link_type=abstract

ORGANIZED BY THE HELLENIC PHYSICAL SOCIETY WITH THE COOPERATION OF THE PHYSICS DEPARTMENTS OF GREEK UNIVERSITIES: 7th Internatio

Physics

Sunspots, Solar Flares, Radio Sources (Astronomical), Solar Corona, Sun Spots, Solar Cycles, Flares, Solar Electromagnetic Emission, Coronal Mass Ejection

Scientific paper

We investigate the relationship of metric type III radio bursts obtained with radio spectrograph ARTEMIS IV (20-650 MHz) in Thermopylae, to GOES SXR/Ha and SOHO/LASCO CMEs within the period of intense activity 20 October to 5 November 2003. Our sample consists of 123 type III radio bursts, 115 SXR Flares (mostly C-type) and 12 CMEs. 69% of type III bursts are coincident in time with SXR Flares, while the rest 31% were detected between successive SXR flux maxima and though not always in the same active region as the SXR Flare, thereby labeled as SXR Less. The lack of SXR enhancement in SXR less type III bursts was probably the result of increased SXR background which prevented detection. It is found also, that 62% of the Flares are associated with type III radio bursts. Furthermore, we study the characteristic type III parameters i.e. start frequency, frequency band and duration as well as the SXR Flare parameters i.e. Flux, Duration, Apparent Area, rise time, decay time and their ratio. Finally, we tried to investigate any characteristic variation occurred because of the different morphology of the three major active regions, 484, 486 and 488 of that period.

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