Loop Morphology and Flows and their Relation to the Magnetic Field

Details Loop Morphology and Flows and their Relation to the Magnetic Field Loop Morphology and Flows and their Relation to the Magnetic Field

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aspc..397..196t&link_type=abstract

First Results From Hinode ASP Conference Series, Vol. 397, Proceedings of the conference held 20-24 August, 2007, at Trinity Col

Astronomy and Astrophysics

Astronomy

Scientific paper

In November 2006 we obtained several rasters of a large sunspot and its trailing region using the SUMER spectrometer on SOHO. The observations consist of spectroheliograms in the continuum around 142 nm and in several spectral lines formed between 80000 K and 0.6 MK, covering the temperature range from the chromosphere to the lower corona. The observed profiles provide LOS velocity and Doppler width maps. TRACE images in the EUV passbands and in the 160 nm continuum provide a clear picture of the coronal loops and the chromosphere near their footpoints. The same target was also observed by all the instruments aboard Hinode and, in particular, by the SOT spectro-polarimeter measuring the photospheric magnetic vector. We combined SOT and MDI data (covering a larger FOV) to infer the coronal magnetic field of the active region by a nonlinear force-free field extrapolation. The observed radiance and velocity patterns at the various heights/temperatures throughout the solar atmosphere are compared with the field topology.

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