English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Under the assumption that the photospheric quiet-Sun magnetic field isturbulent, the cancellation function has previously been used to estimate thetrue, resolution-independent mean, unsigned vertical flux$<|B_z|>_{\mathrm{true}}$. We show that the presence of network elements,noise, and seeing complicate the measurement of accurate cancellation functionsand their power-law exponents $\kappa$. Failure to exclude network elementspreviously led to too low estimates of both the cancellation exponent $\kappa$and of $<|B_z|>_{\mathrm{true}}$. However, both $\kappa$ and$<|B_z|>_{\mathrm{true}}$ are over-estimated due to noise in magnetograms.While no conclusive value can be derived with data from current instruments,our {\it Hinode}/SP results of $\kappa\lessapprox0.38$ and$<|B_z|>_{\mathrm{true}}\lessapprox 270 $gauss can be taken as upper bounds.

Instrumental and Observational Artifacts in Quiet Sun Magnetic Flux Cance llation Functions