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      Solar neutrino flare, megaton neutrino detectors and human space journey

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          Abstract

          The largest solar flare have been recorded in gamma flash and hard spectra up to tens GeV energy. The present building and upgrade of Hyper- Kamiokande (HK) in Japan and Korea, (as well as Deep Core, PINGU) Megatons neutrino detectors do offer a novel way to detectable trace of solar flares: their sudden anti-neutrino (or neutrino) imprint made by proton scattering and pion decays via Delta resonance production on solar corona foot-point. These signals might be observable at largest flare by HK via soft spectra up to tens-hundred MeV energy and by IceCube-PINGU at higher, GeVs energies. We show the expected rate of signals for the most powerful solar flare occurred in recent decades extrapolated for future Megaton detectors. The neutrino solar flare detection with its prompt alarm system may alert astronauts on space journey allowing them to hide themselves into inner rocket container surrounded by fuel or water supply. These container walls are able to defend astronauts from the main lethal (the dominant soft component) radiation wind due to such largest solar flares.

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          The 6 September 2017 X‐Class Solar Flares and Their Impacts on the Ionosphere, GNSS, and HF Radio Wave Propagation

          Abstract On 6 September 2017, the Sun emitted two significant solar flares (SFs). The first SF, classified X2.2, peaked at 09:10 UT. The second one, X9.3, which is the most intensive SF in the current solar cycle, peaked at 12:02 UT and was accompanied by solar radio emission. In this work, we study ionospheric response to the two X‐class SFs and their impact on the Global Navigation Satellite Systems and high‐frequency (HF) propagation. In the ionospheric absolute vertical total electron content (TEC), the X2.2 SF caused an overall increase of 2–4 TECU on the dayside. The X9.3 SF produced a sudden increase of ~8–10 TECU at midlatitudes and of ~15–16 TECU enhancement at low latitudes. These vertical TEC enhancements lasted longer than the duration of the EUV emission. In TEC variations within 2–20 min range, the two SFs provoked sudden increases of ~0.2 TECU and 1.3 TECU. Variations in TEC from geostationary and GPS/GLONASS satellites show similar results with TEC derivative of ~1.3–1.7 TECU/min for X9.3 and 0.18–0.24 TECU/min for X2.2 in the subsolar region. Further, analysis of the impact of the two SFs on the Global Navigation Satellite Systems‐based navigation showed that the SF did not cause losses‐of‐lock in the GPS, GLONASS, or Galileo systems, while the positioning error increased by ~3 times in GPS precise point positioning solution. The two X‐class SFs had an impact on HF radio wave propagation causing blackouts at <30 MHz in the subsolar region and <15 MHz in the postmidday sector.
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            Detecting Solar Neutrino Flares and Flavors

            D. Fargion (2003)
            Intense solar flares originated in sun spots produce high energy particles (protons, \(\alpha\)) well observable by satellites and ground-based detectors. The flare onset produces signals in different energy bands (radio, X, gamma and neutrons). The most powerful solar flares as the ones occurred on 23 February 1956, 29 September 1989 and the more recent on October 28th, and the 2nd, 4th, 13th of November 2003 released in sharp times the largest flare energies (\({E}_{FL} \simeq {10}^{31}\div {10}^{32} erg). The high energy solar flare protons scatter within the solar corona and they must be source of a prompt neutrino burst through the production of charged pions. Later on, solar flare particles hitting the atmosphere may marginally increase the atmospheric neutrino flux. The prompt solar neutrino flare may be detected in the largest underground \)\nu\( detectors. Our estimate for the October - November 2003 solar flares gives a number of events above the unity. The electron/muon \)\nu\( signals and spectra may reflect the neutrino flavour mixing. A surprising tau appearance may occur for a hard {E}_nu_mu}} \to {E}_{{\nu}_{\tau}}\simeq> 4 GeV\)) flare spectra.
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              Author and article information

              Journal
              06 September 2018
              Article
              1809.02004
              f2aa20d5-ba37-4e72-b307-e63434021c36

              http://arxiv.org/licenses/nonexclusive-distrib/1.0/

              History
              Custom metadata
              15 pages, 12 figures
              astro-ph.HE

              High energy astrophysical phenomena
              High energy astrophysical phenomena

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