Large ground level events in solar cycle 22 and some peculiarities of relativistic proton acceleration

Vashenyuk, É. V.; Miroshnichenko, L. I.; Sorokin, M. O.; Pérez‐Peraza, J.; Gallegos, A.

doi:10.1016/0273-1177(94)90531-2

Cited by 12 publications

(6 citation statements)

References 5 publications

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“…The peculiarities of many GLEs from Table 2.1 were analyzed in some details by Vashenyuk et al (1993Vashenyuk et al ( , 1994Vashenyuk et al ( , 2008, Miroshnichenko et al (1995aMiroshnichenko et al ( , b, c, 1996, Perez-Peraza et al (2008). In addition to a visual intercomparison of the intensitytime profiles measured by different NMs for the same event, there were used so-called vT m -technique (v is the particle velocity and T m -the time of maximum increase at 1 AU) proposed by Wibberenz (1973, 1974), and the distribution of GLEs on a specific parameters T 1/2 -the width of intensity-time profile at its half height .…”

Section: Evidence Of Two-phase Structurementioning

confidence: 99%

“…The corresponding estimate of the parameter A m for the event of October 22, 1989 is A m % 2.0 AU, hence it follows that the value of Λ || % 0.5 AU is considerably larger than that for the event of September 29, 1989. A detailed analysis by Vashenyuk et al (1993Vashenyuk et al ( , 1994, however, clearly demonstrated a limitation of traditional diffusion approach to the study of the intensity-time profiles in such a complicated SPE as the GLE of September 29, 1989.…”

Section: Specific Features Of Particle Releasementioning

confidence: 99%

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Solar Cosmic Rays

Miroshnichenko

2015

Astrophysics and Space Science Library

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Section: Evidence Of Two-phase Structurementioning

confidence: 99%

Section: Specific Features Of Particle Releasementioning

confidence: 99%

Solar Cosmic Rays

Miroshnichenko

2015

Astrophysics and Space Science Library

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“…The method is based on a modern conception of the standard‐kind method with a new yield function and inversion method. In fact, they distinctly showed the presence of an “early” phase and a “late” phase in the ground NM data during the GLE71, which in some measure could be considered as equivalent to the PC and DC that were put in evidence long ago by the group of Apatity (e.g., Miroshnichenko et al, ; Vashenyuk et al, , , , , , , Vashenyuk, Balabin, et al, , Vashenyuk, Miroshnichenko, et al, ). Their early phase is illustrated in Figure , corresponding to the angle‐averaged integrated fluency from 02:00 to 02:40 UT.…”

Section: Energy Spectrum Of the 17 May 2017mentioning

confidence: 93%

Source Energy Spectrum of the 17 May 2012 GLE

et al. 2018

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Among the several GLEs (ground level enhancements) that have presumptuously occurred in the period 2012–2015, the 17 May 2012 is that which is more widely accepted to be a GLE, in view of the high number of high‐latitude neutron monitor stations that have registered it. In spite of the small amplitude, it was more prominent of the predicted GLE's of the present decade (Pérez‐Peraza & Juárez‐Zuñiga, 2015, https://doi.org/10.1088/0004-637X/803/1/27). However, the lack of latitude effect makes it difficult to study the characteristics of this event in the high‐energy extreme of the spectrum. Nevertheless, several outstanding works have been able to derive observational spectra at the top of the Earth atmosphere for this peculiar GLE. Some of these works find that the flow of protons is characterized by two components. Quite a great number of works have been published in relation with observational features obtained with different instrumentation, but the source phenomena, regarding the generation processes and source physical parameters, have not been scrutinized. The main goal of this work is to look at such aspects by means of the confrontation of the different approaches of the observational spectra with our analytical theoretical spectra based on stochastic acceleration and electric field acceleration from reconnection processes. In this way, we derive a set of parameters which characterize the sources of these two GLE components, leading us to propose possible scenarios for the generation of particles in this particular GLE event.

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“…That was done by solving the momentum-diffusion equation by means of the WKBJ method. Since 1992 we have studied [4][5][6][7][8][9][10][11] different kinds of turbulence that presumably can co-exist at the Sun in the sources of SEPs: the MHD modes (slow, fast and Alfvén ones), Langmuir and Bernstein waves. The main attention is paid to the recent super-event of 20 January 2005. and macroscopic processes, respectively).…”

Section: Different Types Of Plasma Turbulence In the Process Of Solarmentioning

confidence: 99%

“…The plausible source and acceleration parameters for some GLEs of the 22-23 solar cycles were derived in [4][5][6][7][8][9][10][11] from the confrontation of theoretical spectra [3,10] with observed ones for both components: the DC vs. stochastic acceleration and the PC vs. deterministic acceleration. The plausible source and acceleration parameters for some GLEs of the 22-23 solar cycles were derived in [4][5][6][7][8][9][10][11] from the confrontation of theoretical spectra [3,10] with observed ones for both components: the DC vs. stochastic acceleration and the PC vs. deterministic acceleration.…”

Section: Different Types Of Plasma Turbulence In the Process Of Solarmentioning

confidence: 99%

Different Types of Plasma Turbulence in the Process of Solar Particle Acceleration

Pérez‐Peraza¹,

Miroshnichenko²,

Vashenyuk³

et al. 2006

AIP Conference Proceedings

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Within the frame of solar cosmic ray (SCR) energy spectra, we present the results of a study of different kinds of turbulence that presumably can co-exist at the Sun in the sources of accelerated particles. On basis of a two-source model of particle generation, one of which is associated with an expanding magnetic loop, we applied the transport equation including adiabatic losses simultaneously with the stochastic acceleration process. Observations show that there are two different populations during some SCR events. One of them, the so-called "Delayed Component" (DC), may be correctly described by stochastic acceleration. The second one, the so-called "Prompt Component" (PC) seems to be described by the deterministic acceleration process in large-scale coronal structures (magnetic neutral current sheets). Co-lateral inferences are obtained for a series of large solar events (, adiabatic cooling is negligible. Qualitative inferences point toward a dominated Alfvén turbulence, at least, during the events of 28 October 2003. Our results also provide a new support to the existence of two relativistic particle populations in some SCR events.

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Large ground level events in solar cycle 22 and some peculiarities of relativistic proton acceleration

Cited by 12 publications

References 5 publications

Solar Cosmic Rays

Solar Cosmic Rays

Source Energy Spectrum of the 17 May 2012 GLE

Different Types of Plasma Turbulence in the Process of Solar Particle Acceleration

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