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

Aims: We investigate the temporal evolution of magnetic flux emergence in thequiet Sun atmosphere close to disk center. Methods: We combine high-resolutionSoHO/MDI magnetograms with TRACE observations taken in the 1216 {\AA} channelin order to analyze the temporal evolution of an emerging small-scale magneticloop and its traces in the chromosphere. Results: At first place, we findsignatures of flux emergence very close to the edge of a supergranular networkboundary located at disk center. The new emerging flux appears first in the MDImagnetograms in form of an asymmetric bipolar element, i.e. the patch withnegative polarity is roughly two-times weaker than the corresponding patch withopposite polarity. The average values of magnetic flux and magnetic fluxdensities reach 1.6 x 10^18 Mx, -8.5 x 10^17 Mx, and 55 Mx cm^-2, -30 Mx cm^-2,respectively. The spatial distance between the opposite polarity patches of theemerged feature increases from about 2.5" to 5.0" during the lifetime of theloop which was not longer than 36 min. A more precise lifetime-estimate of thefeature was not possible because of a gap in the temporal sequence of the MDImagnetograms. The chromospheric response to the emerged magnetic dipole occurs~ 9 minutes later with respect to the photospheric magnetograms. It consists ofa quasi-periodic sequence of time-localized brightenings visible in the 1216{\AA} TRACE channel apparent for ~ 14 minutes and being co-spatial with theaxis connecting the two patches of opposite magnetic polarity. Conclusions: Weidentify the observed event as a small-scale magnetic loop emerging atphotospheric layers and subsequently rising up to the chromosphere. We discussthe possibility that the fluctuations detected in the chromospheric emissionprobably reflect magnetic field oscillations which propagate to thechromosphere in form of waves.

Evidence of quiet Sun chromospheric activity related to an emerging small-scale magnetic loop