Abstract
The photospheric magnetic field outside of active regions and the network has a ubiquitous and dynamic lineof-
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.
| Original language | Undefined/Unknown |
|---|---|
| Pages (from-to) | L177-L180 |
| Number of pages | 4 |
| Journal | Astrophysical Journal |
| Volume | 659 |
| Issue number | 2 |
| Publication status | Published - 2007 |