The Redshifted Network Contrast - Signature of Coronal Convectio

Details The Redshifted Network Contrast - Signature of Coronal Convectio The Redshifted Network Contrast - Signature of Coronal Convectio

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008espm...12.2.92c&link_type=abstract

"12th European Solar Physics Meeting, Freiburg, Germany, held September, 8-12, 2008. Online at http://espm.kis.uni-freiburg.de/,

Physics

Scientific paper

Observations and interpretations of red- and/or blueshifted emission lines from cosmic objects are crucial to understanding the physical processes at work there. The ubiquituous net redshifts of solar transition region (TR) emission lines are known since the Skylab era. Brekke et al. and Chae et al. independently verified this result by analyzing the high spectral resolution observations from the SUMER/SoHO instrument. Both these groups found similar results for the quantitative dependence of the net redshift on line formation temperatures from 30 000 K to 1 MK. To our knowledge, however, a satisfactory physical explanation of the redshift is still a matter of debate. We present a new method to explain the TR red shift, which is based on the radiance-redshift relationship, and which employs the redshift of the network contrast as compared to the position of the emission line itself. In contrast to the earlier work, our indirect method is unique in several ways namely,
(i) it does not require a good wavelength calibration and thus avoids related problems,
(ii) it is independent of the knowledge of the exact rest wavelength, and
(iii) it intimately relies on the physical processes in the solar atmosphere.

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