Active Region Magnetic Field Line Twist and Source of Coronal Magnetic Helicity.

Details Active Region Magnetic Field Line Twist and Source of Coronal Magnetic Helicity. Active Region Magnetic Field Line Twist and Source of Coronal Magnetic Helicity.

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.2401b&link_type=abstract

American Astronomical Society Meeting 210, #24.01; Bulletin of the American Astronomical Society, Vol. 39, p.128

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Magnetic helicity is an important quantity which measures how the magnetic field lines are twisted and sheared. Recently it has become possible to measure the flux of magnetic helicity in active regions using the observational data. These observed helicity fluxes may arise due to the twist in the emerging active region flux tubes or it may come from the photospheric shearing motion. Here, we decompose the helicity flux into two different contributions called spin and braiding. These components typically come from twist and writhe helicity of a sub-photospheric flux tube anchored to the regions. The spin helicity of a given region quantifies the mean rotation rate of motion internal to that region and braiding helicity is injected by the motions of whole
regions about one another. The injected helicity flux due to spin and braiding motion leads to the coronal magnetic field line twist. The twist determined from vector magnetograms can be used to estimate the total helicity content of the coronal field at one time. The rate of change of this helicity estimate can be compared to the total helicity flux as well as its spin and braiding component. We make such a comparison for several active regions.

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