Why Some Fast and Wide Coronal Mass Ejections are Radio-quiet?

Details Why Some Fast and Wide Coronal Mass Ejections are Radio-quiet? Why Some Fast and Wide Coronal Mass Ejections are Radio-quiet?

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.5801g&link_type=abstract

American Astronomical Society Meeting 210, #58.01; Bulletin of the American Astronomical Society, Vol. 39, p.167

Astronomy and Astrophysics

Astronomy

Scientific paper

The radio-quiet CMEs lack type II radio burst association in the metric and decameter-hectometric (DH) wavelengths. We compiled CMEs faster than 900 km/s and wider than 60 degrees and checked against metric and interplanetary type II bursts and found that about one third of them were radio-quiet. We compared the radio-quiet CMEs with the radio-loud ones occurring over the same study period (1996-2005). The radio-quiet and radio-loud CMEs had average speeds of 1129 and 1524 km/s, respectively bracketing the average speed of all FW CMEs (1303 km/s). The width distributions also showed a similar behavior: the fraction of halo and partial halo CMEs was the largest for the radio-loud CMEs (54%), smallest for the radio-quiet CMEs (18%) and intermediate for all fast and wide CMEs (42%). The majority of radio-quiet CMEs (55%) were back-sided; most of the frontsided ones also originated close to the limb. This is in contrast to the radio-loud CMEs which originated generally on the disk with only a small fraction (13%) was back-sided. The average flare size was also slightly smaller for the radio-quiet CMEs compared to that of radio-loud CMEs. Back-sided and limb CMEs have only part of the shock surface visible to the observer. This seems to be an important factor deciding whether a CME is radio quiet.

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