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Seething Horizontal Magnetic Fields in the Quiet Solar Photosphere View all abstracts by submitter

John Harvey   Submitted: 2007-02-15 12:08

The photospheric magnetic field outside of active regions and the network has a ubiquitous and dynamic line-of-sight component that strengthens from disk center to limb as expected for a nearly horizontal orientation. This component shows a striking time variation with an average temporal rms near the limb of 1.7 G at ~3'' resolution. In our moderate resolution observations the nearly horizontal component has a frequency variation power law exponent of -1.4 below 1.5 mHz and is spatially patchy on scales up to ~15 arcsec. The field may be a manifestation of changing magnetic connections between eruptions and evolution of small magnetic flux elements in response to convective motions. It shows no detectable latitude or longitude variations.

Authors: J. W. Harvey, D. Branston, C. J. Henney, C. U. Keller, and the SOLIS and GONG Teams
Projects: None

Publication Status: ApJL (submitted)
Last Modified: 2007-02-16 10:16
Go to main E-Print page  Estimation of spicule magnetic field using observed kink waves  The Ribbon-Like Hard X-Ray Emission in a Sigmoidal Solar Active Region  Edit Entry  Delete Entry 

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