Open and closed magnetic structures in the transition region

Details Open and closed magnetic structures in the transition region Open and closed magnetic structures in the transition region

Oct 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.505..525p&link_type=abstract

In: SOLMAG 2002. Proceedings of the Magnetic Coupling of the Solar Atmosphere Euroconference and IAU Colloquium 188, 11 - 15 Jun

Computer Science

Sun: Transition Region, Sun: Corona

Scientific paper

To trace back the origin of the solar wind to the transition region and chromosphere it is of importance to distinguish between magnetically open and closed regions. As it is not yet possible to measure coronal fields with the required accuracy, one has to fall back on interpreting the observed spectra. If heated by the same energy flux a magnetically closed region should be significantly denser than an open region. This is because the solar wind carries away up to 90% of the energy input. Therefore the emission is dominated by closed structures almost everywhere on the Sun. The noticeable difference in density of open and closed regions allows to distinguish open and closed regions by means of spectroscopy. As the non-thermal broadening, e.g. due to waves, is larger in a less dense plasma, one expects two-component spectral profiles in areas where open and closed regions are not resolved spatially: a narrow intense line core from the dense low coronal loops and a broad weaker tail component from coronal funnels. The latter ones might be either feet of large less dense loops or the base of the solar wind. This paper will present results on the spectroscopic deconvolution of magnetically open and closed regions, e.g., wave transport of energy in the coronal funnels. The results will also be related to stellar transition region observations.

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