On the status of the sunspot and magnetic cycles in the galactic cosmic ray intensity

2015

J. Phys.: Conf. Ser.

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.

Section: The Illustrationsmentioning

confidence: 99%

“…The horizontal bands between the columns mark the latitudes where the TPE coefficients (the solar wind and drift velocities and diffusion tensor) greatly change (see [3,12,13,14]) for details. these terms are proportional to A.…”

Section: The Illustrationsmentioning

confidence: 99%

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

2015

J. Phys.: Conf. Ser.

“…On the other hand, on the basis of the analysis of data on solar and heliospheric characteristics important for GCR propagation, we examined the formation of the heliosphere and its structure, the role of heliospheric boundary layersadjacent to the Sun (in [Krainev, Webber, 2004], we called it the basement of the heliosphere) and adjacent to interstellar space (the so-called inner heliosheath). First, when discussing the effect of the two branches of solar activity on the heliospheric characteristics important for GCR, the consideration was largely qualitative [Krainev et al, 2013]. Then, using the model of potential magnetic field with source surface (see [Altschuler, Newkirk, 1969;Schatten et al, 1969] and references in [Hoeksema, 1984]), we determined the form of magnetic field neutral lines on the source surface, which after the line is extended by the solar wind in the heliosphere yields an acceptable model of the form of the heliospheric current sheet [Krainev, Kalinin, 2010].…”

Section: Introductionmentioning

confidence: 99%

Manifestations of Two Branches of Solar Activity in the Heliosphere and GCR Intensity

Solar-Terrestrial Physics

2019

This paper provides insight into heliospheric processes and galactic cosmic ray (GCR) modulation occurring due to the presence of two branches of solar activity in this solar layer. According to the topology of solar magnetic fields, these branches are called toroidal (active regions, sunspots, flares, coronal mass ejections, etc.) and poloidal (high-latitude magnetic fields, polar coronal holes, zonal unipolar magnetic regions, etc.). The main cause of different manifestations of the two branches on the solar surface and in the heliosphere — the layer at the base of the heliosphere in which the main energetic factor is the magnetic field — is formulated. In this case, the magnetic fields of the poloidal branch, which have a larger scale but a lower intensity, gain an advantage in penetrating into the heliosphere. A connection is shown between the poloidal branch and the heliospheric characteristics (solar wind velocity field, size of the heliosphere, form of the heliospheric current sheet, regular heliospheric magnetic field and its fluctuations) that, according to modern notions, determine GCR propagation in the heliosphere.

“…С другой стороны, на основании анализа данных о солнечных и гелиосферных характеристиках, важных для распространения ГКЛ, проводилось исследование процесса образования гелиосферы и ее строения, роли гелиосферных пограничных слоевприлегающего к Солнцу (в работе мы назвали его подложкой гелиосферы) и прилегающего к межзвездному пространству (так называемый внутренний гелиошит). Сначала при обсуждении влияния двух ветвей солнечной активности на важные для ГКЛ гелиосферные характеристики рассмотрение было в основном качественным [Krainev et al, 2013]. Затем с использованием модели потенциального магнитного поля с поверхностью источника (см.…”

Section: Introductionunclassified

Manifestations of Two Branches of Solar Activity in the Heliosphere and GCR Intensity

Solnechno-Zemnaya Fizika

2019