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/

Zendy Plus

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

Zendy Tools

Zendy Open

Taking advantage of the absence of solar activity in the recent 2008-9 epoch(no spots, few faculae), we have made equatorial and meridian disk scans incontinua from 3129 {\AA} to 46700 {\AA}. Averaging 20 scans at each wavelengthto suppress granulation, which takes a total of 35 minutes, we achieve a systemnoise level of 0.01%. We believe this noise level is a record low, not becauseof instrument improvements, but simply because of observing procedures and thecooperation of the Sun and sky. The observed solar fluctuations significantlyexceed the noise and range from 0.3% at 3130 {\AA}, 0.05% at 34000 {\AA}, to0.06% at 46700 {\AA} near disk center. These fluctuations (corresponding toabout 3 K) presumably arise from the incomplete averaging of granulation.Standard solar models for limb darkening fit the data for true continuumregions reasonably well. No significant differences are seen between scandirections (EW, N-S). Perhaps our results can serve as a template for exoplanetdetection by the transit of quiet G2V-like stars.

Uniformity of the quiet solar disk: 3130 - 46700 {\AA}