Location of Coronal and IP Type II Burst Source Regions from Radio and White-light Observations

Details Location of Coronal and IP Type II Burst Source Regions from Radio and White-light Observations Location of Coronal and IP Type II Burst Source Regions from Radio and White-light Observations

Publishing date

Dec 2011

URL

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh23a1947m&link_type=abstract

Journals

American Geophysical Union, Fall Meeting 2011, abstract #SH23A-1947

Science

Astronomy and Astrophysics

Field

Astrophysics

Additional info 3

[2101] Interplanetary Physics / Coronal Mass Ejections, [2139] Interplanetary Physics / Interplanetary Shocks, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7534] Solar Physics, Astrophysics, And Astronomy / Radio Emissions

Type

Scientific paper

Abstract

We present our preliminary results on the locations of source regions of the type II radio bursts in the metric (m) and dekameter-hectometric (DH) wavelength range. Type II bursts are occasionally observed to consist of two temporally overlapping lanes of metric and DH bursts. It has been suggested that the DH-component could be associated with a CME-driven shock and the m-component with a blast wave or unknown source, or that the DH-component originates from the shock nose and the m-component from the shock flanks. In our study we used time-height measurements of the associated coronal mass ejections (CMEs) to estimate speeds at various position angles (PAs) along the CME front. We also estimated plasma densities at the same PAs in the corona from inversion of polarized brightness (pB) images of SOHO/LASCO coronagraphs. These measurements suggest that both the m and DH-components can be explained reasonably well with a single CME-driven shock as their source.

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