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Seething Horizontal Magnetic Fields in the Quiet Solar Photosphere

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Published 2007 March 27 © 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A.
, , Citation J. W. Harvey et al 2007 ApJ 659 L177 DOI 10.1086/518036

1538-4357/659/2/L177

Abstract

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''. 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.

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10.1086/518036