Emergence of Helical Flux and the Formation of an Active Region Filament Channel

Details Emergence of Helical Flux and the Formation of an Active Region Filament Channel Emergence of Helical Flux and the Formation of an Active Region Filament Channel

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.0910l&link_type=abstract

American Astronomical Society, SPD meeting #40, #9.10; Bulletin of the American Astronomical Society, Vol. 41, p.818

Astronomy and Astrophysics

Astronomy

Scientific paper

We present comprehensive observations from Hinode/SOT and TRACE of the formation and evolution of a filament channel within NOAA Active Region 10978. We employ sequences of Hinode spectro-polarimeter maps of the active region, accompaning Hinode NFI magnetograms in the Na I D1 line, Hinode BFI filtergrams in the Ca II H-line and G-band, and TRACE Fe IX 171 [[Unable to Display Character: Ǻ]] image sequences. The development of the channel resembles qualitatively that presented by Okamoto et al. (2008,2009) in that many indicators that point to the emergence of a pre-existing sub-surface flux rope. The formation takes place rapidly in the course of a few hours, and the filament channel gradually shrinks over the following two days. Particular to this filament channel is the observation of a segment of horizontal, weak (500 Gauss) flux that is not flanked by stronger field, opposite polarity flux. Because this isolated horizontal field is observed in photospheric lines, we infer that it is unlikely that the channel formed as a result of reconnection in the higher layers of the atmosphere. Furthermore, correlation tracking of granulation in the G-band presents no evidence for either systematic flows toward the channel or systematic shear flows along it. The absence of these flows reinforces the picture of an emerging flux rope as the origin of this filament channel.

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