Effect of the IMF neutral surface on north-south anisotropy of cosmic rays

Krymsky, G. F.; Krivoshapkin, P. A.; Mamrukova, V. P.; Gerasimova, S. K.

doi:10.1134/s0016793206060041

Cited by 17 publications

(20 citation statements)

References 5 publications

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“…Assuming also a slow time evolution and particle velocities much larger than the medium velocity we come to the standard transport equation for cosmic rays (Krymsky 1964;Parker 1965;Dolginov & Toptygin 1966;Gleeson & Axford 1969):…”

Section: Basic Equationsmentioning

confidence: 99%

“…Progress in cosmic ray astrophysics has been made with the introduction of the transport equation for cosmic rays (Krymsky 1964;Parker 1965;Dolginov & Toptygin 1966;Gleeson & Axford 1969). It was successfully applied to many astrophysical problems: cosmic ray modulation in the solar wind, acceleration of particles at shock fronts, cosmic ray propagation in the Galaxy etc.…”

Section: Introductionmentioning

confidence: 99%

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Hemispherical transport equation: modeling of quasiparallel collisionless shocks

Zirakashvili¹

2007

A&A

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Using a so-called hemispherical model we derive a general transport equation for cosmic ray and thermal particles scattered in pitch angle by magnetic inhomogeneities in a moving collisionless plasma. The weak scattering through 90 degrees results in isotropic particle distributions in each hemisphere. The consideration is not limited by small anisotropies and by the condition that particle velocities are higher than characteristic flow velocity differences. For high velocities and small anisotropies the standard cosmic ray transport equation is recovered. We apply the equations derived for investigation of injection and acceleration of particles by collisionless shocks.

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Section: Basic Equationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Hemispherical transport equation: modeling of quasiparallel collisionless shocks

Zirakashvili¹

2007

A&A

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“…As to the specific mechanism how the form of the HCS influences the galactic cosmic ray (GCR) intensity, the great majority of the specialists agree that it is the fast drift of the particles along the HCS itself [3,4], although there is an opinion that the HCS only changes the important for GCR properties of the heliosphere (the strength of the magnetic field [5] or the diffusion coefficient [6] in the sector-structure zone of the heliospheric magnetic field). We believe that the first mechanism is the main one, although both effects should be considered, however using the HCS model much more realistic than a definitely oversimplified so called tiled current sheet (TCS) model, [3], usually used in the cosmic ray studies.…”

Section: Introductionmentioning

confidence: 99%

Models of the infinitely thin global heliospheric current sheet

Крайнев¹,

Калинин²,

Maksimović³

et al. 2010

AIP Conference Proceedings

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On the models of the global heliospheric current sheet with the finite thickness and all three components of the magnetic field AIP Conf.Abstract. The different models of the infinitely thin global heliospheric current sheet with small (< 5) number of parameters are considered. It is shown that the form of the current sheets calculated using the Wilcox Solar Observatory (WSO) model, the main source of our knowledge of this form, is rather complicated and none of the models considered adequately describe these current sheets. The characteristics of the magnetic drift velocity and the distribution of the galactic cosmic ray intensity are calculated both for the widely used model of the tilted current sheet and for the WSO current sheet. It is demonstrated that the dependence of both drift velocity and intensity distribution on the model used is significant.Keywords: solar magnetic field, heliospheric magnetic field, heliospheric current sheet, models of the heliospheric current sheet, galactic cosmic rays, modeling galactic cosmic ray intensity PACS: 96.60.Hv, 96.50.Bh, 96.50.sh

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“…The TPE for the cosmic ray intensity J in its conventional form was derived by Parker [4,5], Krymsky [6], Jokipii et al [7] (if we list few names) in the first twenty years of the theoretical study of the GCR modulation. Usually it deals with the distribution function f (⃗ r, p, t) = J(⃗ r, T, t)/p 2 , where p is the momentum of particles.…”

Section: The Boundary-value Problemmentioning

confidence: 99%

“…where (7,8) are equal to their counterparts in (5,6) in the nodes of the grid, while AX X i± 1 2 in (7) is equal to AXX in (6) at halfway between nodes X i and X i±1 . The indices j, k are not repeated in (7), as well as i, j in (8).…”

Section: Solving the Boundary-value Problemmentioning

confidence: 99%

On the method of the GCR partial intensities related to the main physical processes of solar modulation

Крайнев

2015

J. Phys.: Conf. Ser.

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Abstract. We discuss in more details the earlier suggested method to decompose the calculated GCR intensity into the partial intensities connected with the main physical processes (the diffusion, convection, adiabatic cooling and magnetic drift) of the solar modulation. The expressions for the partial intensities connected with the convection and adiabatic cooling are improved and some results are illustrated. IntroductionThis work deals with some additional calculations that can be made in the course of the usual numerical solution of the boundary problem for the GCR intensity. The aim of these calculations is to improve our understanding of behavior of this intensity in the heliosphere.But first, why are we not fully satisfied with the conventional approach and look for some additional means? Of course, all physics of modeling the GCR modulation lies in the Transport Partial differential Equation (TPE) with the boundary and "initial" conditions for the intensity and in the models of the TPE coefficients used. So one solves the boundary problem, compares the results with the observations and makes the conclusions about the degree of understanding of the modulation process. However, observations of the GCR intensity and heliospheric characteristics are very incomplete; besides, even in the simplest case the calculated GCR differential intensity J(⃗ r 0 , T 0 , t 0 ) for the position ⃗ r 0 , energy T 0 and time t 0 is the result of complex interplay between several main physical processes (the diffusion, convection, drift, adiabatic cooling) for all higher energies (T > T 0 ) and in previous moments (t < t 0 ) in the whole heliosphere. And the details of this interplay are still unrevealed in the calculations, only its result. But to understand this interplay, in particular, the contribution of different processes to the calculated intensity, is very interesting and important.In [1, 2] we suggested the method to decompose the calculated GCR intensity into the partial intensities connected with the main physical processes. In [3] the method was applied to understand the mechanisms forming the time profiles of the GCR intensity near the Earth during the last three periods of low solar activity. In this paper, first, we shall briefly discuss the usual process of modeling the GCR intensity and specify which additional calculations could be made and how they can be used for our purpose. Second, the expressions used earlier for the partial intensities connected with the convection and adiabatic cooling will be improved. Then some results will be illustrated and discussed.

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Effect of the IMF neutral surface on north-south anisotropy of cosmic rays

Cited by 17 publications

References 5 publications

Hemispherical transport equation: modeling of quasiparallel collisionless shocks

Hemispherical transport equation: modeling of quasiparallel collisionless shocks

Models of the infinitely thin global heliospheric current sheet

On the method of the GCR partial intensities related to the main physical processes of solar modulation

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