Simultaneous Observation of Solar Neutrons from the International Space Station and High Mountain Observatories in Association with a Flare on July 8, 2014

Muraki, Y.; López, Diego; Koga, Kiyokazu; Kakimoto, F.; Goka, T.; González, L. X.; Masuda, S.; Matsubara, Y.; Matsumoto, Haruhisa; Miranda, P.; Okudaira, O.; Obara, Takao; Salinas, J.; Sako, T.; Shibata, S.; Ticona, R.; Tsunesada, Y.; Galicia, J. F. Valdés; Watanabe, Kyoko; Yamamoto, T.

doi:10.1007/s11207-016-0887-0

Cited by 10 publications

(4 citation statements)

References 36 publications

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“…Assuming that the SAγ flux is produced by hadronic processes, the solar neutron flux recorded by the Fermi-LAT should be similar to the gamma-ray flux (see e.g., SSG1991). Solar neutrons have, in fact, been observed by Earth-bound observatories and correlated with gamma-ray emission during solar flares [51,52].…”

Section: Hypothesis Iii: Solar Neutronsmentioning

confidence: 99%

Unexpected dip in the solar gamma-ray spectrum

Tang

Linden

et al. 2018

Phys. Rev. D

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The solar disk is a bright source of multi-GeV gamma rays, due to the interactions of hadronic cosmic rays with the solar atmosphere. However, the underlying production mechanism is not understood, except that its efficiency must be greatly enhanced by magnetic fields that redirect some cosmic rays from ingoing to outgoing before they interact. To elucidate the nature of this emission, we perform a new analysis of solar atmospheric gamma rays with 9 years of Fermi-LAT data, which spans nearly the full 11-year solar cycle. We detect significant gamma-ray emission from the solar disk from 1 GeV up to 200 GeV. The overall gamma-ray spectrum is much harder (∼ E −2.2 γ ) than the cosmic-ray spectrum (∼ E −2.7 CR ). We find a clear anticorrelation between the solar cycle phase and the gamma-ray flux between 1-10 GeV. Surprisingly, we observe a spectral dip between ∼30-50 GeV in an otherwise power-law spectrum. This was not predicted, is not understood, and may provide crucial clues to the gamma-ray emission mechanism. The flux above 100 GeV, which is brightest during the solar minimum, poses exciting opportunities for HAWC, LHAASO, IceCube, and KM3NeT.

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Section: Hypothesis Iii: Solar Neutronsmentioning

confidence: 99%

Unexpected dip in the solar gamma-ray spectrum

Tang

Linden

et al. 2018

Phys. Rev. D

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“…First, the Solar Energetic Particle (SEP) events that form part of SW hazards are contemplated. In the Mexican latitudes, these are caused by solar flares [75][76][77]. The SCiESMEX considers a SEP event's presence if the particle flux intensity exceeds its average value during the last three hours.…”

Section: Cosmic Rays Perspectivementioning

confidence: 99%

On Some Challenges for National and Global Space Weather Services

Sergeeva,

Gonzalez-Esparza,

Gatica-Acevedo

et al. 2023

Remote Sensing

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Space Weather (SW) hazards are discussed in terms of the operation of national SW services and global SW centers for the International Civil Aviation Organization (ICAO). The definition of threshold values of monitored parameters which are used to identify moderate and severe SW events is one of the critical problems. Due to the lack of both physical data on severe events and user feedback, we tried to approach the problem statistically. In particular, we pursued the answer to the question about what intensity of ionospheric storms and flare effects should be reported by national and global SW entities to their users. We also discussed the possible role of an active region on the Sun, and the cosmic rays’ issues that may be helpful regarding SW operational work. The presented considerations are based on examples of the ionosphere state assessment for the low-latitude American sector with a focus on the Mexican region. This work attempts to argue the possible approaches to resolve the tasks that the SW national services and global centers face.

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“…More recently, Muraki et al [22] reported the simultaneous observation of solar neutrons from the SEDA-NEM instrumend on board the International Space Station [23] and high mountain observatories located in Mt. Chacaltaya, Bolivia, and Mt.…”

Section: A Solar Flaresmentioning

confidence: 99%

“…Thus, a much larger detector would be needed to reach the interesting energy regions for indirect WIMP detection. Imaida et al [91] also developed a neutron detector made by scintillating fibres and a multi-anode photomultiplier, which was operated in space [22,23]. Like SONTRAC, it covers the energy range interesting for solar flares.…”

Section: B Detector Designmentioning

confidence: 99%

Neutron astronomy

Casadei¹

2017

Preprint

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Neutrons travel along straight lines in free space, but only survive for a distance which depends on their energy. Thus, detecting neutrons in space in principle provides directional and distance information. Apart from secondary neutrons produced by cosmic-ray interactions in the Earth atmosphere, which are the dominant background, direct neutron emission is caused by solar flares, with clear time correlation with X-rays, which can be measured from few tens MeV up to few GeV. There is no detectable astrophysical source up to the PeV scale, when neutrons coming from supernova remnants may reach the Earth before decaying. In addition, ultra high energy neutrons are the most plausible explanation for the measured anisotropy of cosmic-ray showers produced in the atmosphere above 10 18 eV. From the GeV to the PeV scale, the expected neutron flux is very low and not too different from the antiproton flux, as the same cosmic-ray collisions with the interstellar medium which can produce antiprotons can also produce neutrons and antineutrons. This background flux of cosmic-ray neutrons is very low and has not yet been detected. Measuring the neutron energy spectrum in space is a very effective way of searching for decays of exotic particles. For example, dark matter could consist of Weakly Interacting Massive Particles (WIMPs), which may annihilate into final states with particle and antiparticle pairs. Consequently, a number of indirect WIMP searches are being carried on, focusing on positron and antiproton spectra. However, no experiment is presently foreseen to look for "bumps" in the neutron energy spectrum, which is virtually background free. Here we consider the implications of a measurement of the neutron energy spectrum in astronomy and astrophysics and list the interesting energy regions in the search for WIMPs.

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Simultaneous Observation of Solar Neutrons from the International Space Station and High Mountain Observatories in Association with a Flare on July 8, 2014

Cited by 10 publications

References 36 publications

Unexpected dip in the solar gamma-ray spectrum

Unexpected dip in the solar gamma-ray spectrum

On Some Challenges for National and Global Space Weather Services

Neutron astronomy

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