Magnetic cancellation and small-scale activity in an AR filament

Details Magnetic cancellation and small-scale activity in an AR filament Magnetic cancellation and small-scale activity in an AR filament

Oct 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.505..223s&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

1

Solar Magnetic Field, Filament

Scientific paper

A long set of observations obtained with the VTT/MSDP spectrograph in September 1998 (8 to 11) allows us to follow the formation of a complex filament in and around a nest of active regions during its disk passage. Continuous shear of magnetic field in this region can explain the formation and the relative stability of the filament structure before the occurrence of a flare which leads to important changes in the magnetic configuration. The corona overlying the region and the flare, as well, is observed by TRACE. The studied filament is stable on long term time scale. However, high spatial and temporal observations obtained in La Palma (SVST) show high Doppler shifts and strong transverse motions of absorbing blobs along the filament. These velocities are directly related to magnetic activity as observed with the SVST. A small scale magnetic analysis shows emergence of MMFs (Moving Magnetic Features) around a decaying sunspot and canceling flux with the neighbor network. Magnetic reconnection could occur and explain the ejection of blobs along the new magnetic field lines. Formation of the transient blobs is discussed.

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