Sinuous Coronal Loops at the Sun [Invited]

Details Sinuous Coronal Loops at the Sun [Invited] Sinuous Coronal Loops at the Sun [Invited]

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mwoc.conf..125p&link_type=abstract

Multi-Wavelength Observations of Coronal Structure and Dynamics -- Yohkoh 10th Anniversary Meeting. Proceedings of the conferenc

Physics

15

Scientific paper

The sinuous coronal loops - sigmoids, first noted in the Skylab X-ray observations in association with a CME, - are commonly observed in Yohkoh soft X-ray telescope (SXT) data. The S-shape of these loops is a manifestation of the helical structure of the coronal magnetic fields and, hence, follows the hemispheric helicity (chirality) rule established for quiescent filaments and photospheric magnetic fields. The forward-S (inverse-S) sigmoids prevail in southern (northern) hemisphere, independent of the solar cycle. Sigmoids are often associated with the CMEs; they exist prior to eruption and disappear after. In addition, active regions that exhibit sinuous loops are more likely to be eruptive than non-sigmoidal regions. Once erupted, sigmoids tend to produce stronger geomagnetic storms, and often the orientation of magnetic field in interplanetary disturbance can be directly linked to the coronal field of a sigmoid. In this talk we review the observational properties of sigmoids, current theoretical models and application of sinuous loops to space weather forecasting.

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