Volume 530, June 2011
|Number of page(s)||4|
|Published online||27 April 2011|
Letters to the Editor
Low polarised emission from the core of coronal mass ejections
Solar-Terrestrial Center of Excellence – SIDC, Royal Observatory of
2 Institute of Geodynamics of the Romanian Academy, 020032 Bucharest, Romania
3 Research Center for Atomic Physics and Astrophysics, Faculty of Physics, University of Bucharest, Romania
4 Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, Germany
5 Astronomical Institute of the Romanian Academy, Bucharest, Romania
6 Skobeltsyn Institute of Nuclear Physics, Moscow State University, Russia
Accepted: 11 April 2011
Aims. In white-light coronagraph images, cool prominence material is sometimes observed as bright patches in the core of coronal mass ejections (CMEs). If, as generally assumed, this emission is caused by Thomson-scattered light from the solar surface, it should be strongly polarised tangentially to the solar limb. However, the observations of a CME made with the SECCHI/STEREO coronagraphs on 31 August 2007 show that the emission from these bright core patches is exceptionally low polarised.
Methods. We used the polarisation ratio method of Moran & Davila (2004) to localise the barycentre of the CME cloud. By analysing the data from both STEREO spacecraft we could resolve the plane-of-the-sky ambiguity this method usually suffers from. Stereoscopic triangulation was used to independently localise the low-polarisation patch relative to the cloud.
Results. We demonstrated for the first time that the bright core material is located close to the centre of the CME cloud. We show that the major part of the CME core emission, more than 85% in our case, is Hα radiation and only a small fraction is Thomson-scattered light. Recent calculations also imply that the plasma density in the patch is 8 × 108 cm-3 or more compared to 2.6 × 106 cm-3 for the Thomson-scattering CME environment surrounding the core material.
Key words: Sun: coronal mass ejections (CMEs) / Sun: filaments, prominences / polarization / techniques: polarimetric
© ESO, 2011
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