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

During our optical monitoring of UV Ceti, iconic late-type flaring star, withhigh temporal resolution using the Russian 6-m telescope in 2008 we detected agiant flare with the amplitude of about 3 magnitudes in $U$-band. Near flaremaximum more than a dozen of spike bursts have been discovered with triangularshapes and durations from 0.6 to 1.2 s and maximal luminosities in the range$(1.5-8)\times10^{27}$ erg~s$^{-1}$. For the half of these events the linearpolarization exceeds 35% with significance better than $5\sigma$. We argue thatthese events are synchrotron emission of electron streams with the energies ofseveral hundred MeV moving in the magnetic field of about 1.4 kG. Emission fromsuch ultrarelativistic (with energies far exceeding 10 MeV) particles is beingroutinely observed in solar flares, but has never been detected from UV Cetitype stars.  This is the first ever detection of linearly polarized optical light from theUV Ceti-type stars which indicates that at least some fraction of the flaringevents on these stars are powered by a non-thermal synchrotron emissionmechanism.

Discovery of the subsecond linearly polarized spikes of synchrotron origin in the UV Ceti giant optical flare