Solar Cosmic Rays

Miroshnichenko, L. I.

doi:10.1007/978-3-319-09429-8

Cited by 31 publications

(12 citation statements)

References 520 publications

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“…* E-mail: koutchmy@iap.fr The primary particles have been deflected by the galactic magnetic field making their trajectory in the interstellar space impossible to follow (Baade and Zwicky 1934;Butt 2009). These particles are then deviated in the much stronger magnetic field of the heliosphere and finally by the magnetic field of our magnetosphere (Dorman 2006;Kahler 1992;Smart and Shea 2009;Miroshnichenko 2015), as illustrated in Fig. 1.…”

Section: Introductionmentioning

confidence: 92%

Observation of galactic cosmic ray spallation events from the SoHO mission 20-yr operation of LASCO

Koutchmy

Tavabi

Urtado

2018

Monthly Notices of the Royal Astronomical Society

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A shower of secondary Cosmic Ray (CR) particles is produced at high altitudes in the Earth's atmosphere, so the primordial Galactic Cosmic Rays (GCRs) are never directly measured outside the Earth magnetosphere and atmosphere. They approach the Earth and other planets in the complex pattern of rigidity's dependence, generally excluded by the magnetosphere. GCRs revealed by images of single nuclear reactions also called spallation events are described here. Such an event was seen on Nov. 29, 2015 using a unique LASCO C3 space coronagraph routine image taken during the Solar and Heliospheric Observatory (SoHO) mission observing uninterruptedly at the Lagrangian L1 point. The spallation signature of a GCR identified well outside the Earth's magnetosphere is obtained for the 1 st time. The resulting image includes different diverging linear "tracks" of varying intensity, leading to a single pixel; this frame identifies the site on the silicon CCD chip of the coronagraph camera. There was no solar flare reported at that time, nor Coronal Mass Ejection (CME) and no evidence of optical debris around the spacecraft. More examples of smaller CR events have been discovered through the 20 years of continuous observations from SoHO. This is the first spallation event from a CR, recorded outside the Earth's magnetosphere. We evaluate the probable energy of these events suggesting a plausible galactic source.

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Section: Introductionmentioning

confidence: 92%

Observation of galactic cosmic ray spallation events from the SoHO mission 20-yr operation of LASCO

Koutchmy

Tavabi

Urtado

2018

Monthly Notices of the Royal Astronomical Society

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“…The energy spectra of these particles provide us with important information for understanding the acceleration process of SCR. [1] For example, an important element to understanding the acceleration process is how high-energy particles are involved in these particles. On the other hand, observation using photon-and light-based telescopes will provide indispensable knowledge relative to understanding the acceleration process of SCR.…”

Section: Introduction: Why We Selected the June 3 2012 Eventmentioning

confidence: 99%

Proton Acceleration by Very Impulsive Flare on June 3, 2012

Kamiya

Koga

Masada

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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On June 3, 2012, a very impulsive solar flare was observed by the GOES, RHESSI and FERMI-LAT satellites. The intensity of the flare was M3.3. The hard X-ray intensity (> 100 keV) rose ≥ 1000 times within one minute and then decayed immediately to the background level (in less than one minute). It was an extremely impulsive flare. By chance, the SEDA-FIB solar neutron detector onboard the International Space Station detected a 5.1σ enhancement due to solar neutrons. Therefore, it provided a good opportunity to investigate the mechanism of instantaneous proton acceleration to a few GeV. Based on the results of a new Monte Carlo calculation, we will show a reasonable proton acceleration model for the June 3, 2012 event. We also reexamined another very impulsive flare observed on June 10, 2010. PoS(ICRC2017)115 PoS(ICRC2017)115 Proton Acceleration by a Very Impulsive Flare K. Kamiya et al.

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“…It was found that solar energetic particles (SEPs) in gradual events are generated at shock fronts accompanying coronal mass ejections (CMEs) in the solar atmosphere [1][2][3]. It is confirmed by close connection between CMEs and SEP increases in gradual events as well as the correspondence of elemental abundances and ionization states of SEP ions and the solar corona plasma, on average [1].…”

Section: Introductionmentioning

confidence: 99%

Influence of region behind the shock front on acceleration of solar energetic particles

Petukhov¹,

Petukhova²,

Stanislav³

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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Acceleration of solar energetic particles by the shock accompanying a coronal mass ejection is considered. Influence of the region behind the shock front on particle acceleration process is investigated. The external boundary of coronal mass ejection and the shock front are specified as the segments of spherical surfaces with the different radii moving in coordination. Nonstationarity of process, spherical symmetry and adiabatic losses of particle energy in the extending environment are considered in the calculation. The propagation velocity of solar wind is determined by the conservation of matter stream taking into account the known distribution of matter density. Scatterings of solar energetic particles are carried out by Alfven waves moving radially from and to the Sun. The parameters determining the coefficient of particle diffusion are chosen taking into account the available results of theoretical calculations and indirect measurements. Influence of the accelerated particles on dynamics of the system and the turbulence level of the magnetic field isn't considered. The performed numerical calculations show that the influence extent of the region behind the shock front on acceleration process is determined by a ratio between coefficients of particle diffusion in regions behind and before the front. In that case when these coefficients are comparable: 1) rate of acceleration significantly decreases; 2) the considerable part of the accelerated particles is behind the shock front.

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Solar Cosmic Rays

Cited by 31 publications

References 520 publications

Observation of galactic cosmic ray spallation events from the SoHO mission 20-yr operation of LASCO

Observation of galactic cosmic ray spallation events from the SoHO mission 20-yr operation of LASCO

Proton Acceleration by Very Impulsive Flare on June 3, 2012

Influence of region behind the shock front on acceleration of solar energetic particles

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