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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

Neutrinos associated with solar flares (solar-flare neutrinos) provideinformation on particle acceleration mechanisms during the impulsive phase ofsolar flares. We searched using the Super-Kamiokande detector for neutrinosfrom solar flares that occurred during solar cycles $23$ and $24$, includingthe largest solar flare (X28.0) on November 4th, 2003. In order to minimize thebackground rate we searched for neutrino interactions within narrow timewindows coincident with $\gamma$-rays and soft X-rays recorded by satellites.In addition, we performed the first attempt to search for solar-flare neutrinosfrom solar flares on the invisible side of the Sun by using the emission timeof coronal mass ejections (CMEs). By selecting twenty powerful solar flaresabove X5.0 on the visible side and eight CMEs whose emission speed exceeds$2000$ $\mathrm{km \, s^{-1}}$ on the invisible side from 1996 to 2018, wefound two (six) neutrino events coincident with solar flares occurring on thevisible (invisible) side of the Sun, with a typical background rate of $0.10$($0.62$) events per flare in the MeV-GeV energy range. No significantsolar-flare neutrino signal above the estimated background rate was observed.As a result we set the following upper limit on neutrino fluence at the Earth$\mathit{\Phi}<1.1\times10^{6}$ $\mathrm{cm^{-2}}$ at the $90\%$ confidencelevel for the largest solar flare. The resulting fluence limits allow us toconstrain some of the theoretical models for solar-flare neutrino emission.

Searching for neutrinos from solar flares across solar cycles 23 and 24 with the Super-Kamiokande detector