Journal ArticleDOI
Calculation of the interplanetary magnetic field based on its value in the solar photosphere
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TLDR
In this paper, the difficulties associated with calculating the parameters of the interplanetary magnetic field (IMF) from solar magnetic data have been considered, and all conventional calculation patterns and available input databases have been analyzed from a unified standpoint.Abstract:
The difficulties associated with calculating the parameters of the interplanetary magnetic field (IMF) from solar magnetic data have been considered. All conventional calculation patterns and available input databases have been analyzed from a unified standpoint. It has been shown that these assumptions and limitations cannot affect the general structure and dependence on cycle of solar and interplanetary data. At the same time, the measured solar field values are underestimated as a result of the magnetograph signal saturation effect. It has been shown that the correction should depend on the heliocentric observation latitude and cycle phase. The correction method responsible for good agreement between the calculated and measured values has been proposed. The created database makes it possible to quantitatively calculate the magnetic fields in the solar wind near the Earth.read more
Citations
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The strength of the sun's polar fields
TL;DR: The magnetic field strength within the polar caps of the sun is an important parameter for both the solar activity cycle and for our understanding of the interplanetary magnetic field as discussed by the authors, and measurements of the polar fields made at the Stanford Solar Observatory using the Fe I line at 525.02 nm.
Journal ArticleDOI
Contrast of Coronal Holes and Parameters of Associated Solar Wind Streams
TL;DR: In this article, it was shown that the contrast of coronal holes, just as their size, determines the velocity of the solar wind streams, and that the correlations with the velocity are rather high (0.70-0.89) especially during the periods of moderate activity, and could be used for everyday forecast.
Journal ArticleDOI
Correlation between the Near-Earth Solar Wind Parameters and the Source Surface Magnetic Field
TL;DR: In this paper, the solar magnetic field at the Earth's projection onto the solar-wind source surface has been calculated for each day over a long time interval (1976-2004) and the data have been compared with the daily mean solar wind velocities and various components of the interplanetary magnetic field near the Earth.
Journal ArticleDOI
Solar-terrestrial storms of October 2003. 2. Five-phase dynamics of the substorm of October 28–30
K. G. Ivanov,A. F. Kharshiladze +1 more
TL;DR: In this paper, a solar-heliospheric storm has five phases based on the storm that occurred in October 2003, and the assumption of the AR configuration adjustment (the second phase) and ordering of disturbances (the third-five phases) during this storm near the subsector boundary between LOFs of identical polarity has been confirmed.
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Magnetic Field as a Tracer for Studying the Differential Rotation of the Solar Corona
O. G. Badalyan,V. N. Obridko +1 more
TL;DR: In this article, the characteristics of differential rotation of the solar corona for the period 1976-2004 were studied as a function of the distance from the center of the Sun, and the results of these calculations make it possible to study the distribution of the rotation periods in the corona depending on distance, time and phase of the cycle.
References
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Journal ArticleDOI
A model of interplanetary and coronal magnetic fields.
TL;DR: Green function solution to the Maxwell equations for interplanetary and coronal magnetic fields above photosphere, considering field at source surface as discussed by the authors, considering magnetic field at the source surface.
Journal ArticleDOI
Magnetic Fields and the Structure of the Solar Corona. I: Methods of Calculating Coronal Fields
TL;DR: In this paper, several different mathematical methods are described which use the observed line-of-sight component of the photospheric magnetic field to determine the magnetic field of the solar corona in the current-free approximation.
Journal ArticleDOI
On potential field models of the solar corona
Y. M. Wang,N. R. Sheeley +1 more
TL;DR: In this article, it is argued that the observed photospheric field should first be corrected for line-of-sight projection and then matched to the radial component of the potential field.
Journal ArticleDOI
Magnetic-field structure of the photospheric network
TL;DR: In this paper, a method is developed to determine the physical parameters of the spatially unresolved photospheric network, where magnetic fluxes are recorded simultaneously in the two FeI lines 5250 and 5247 A, which belong to the same multiplet and have practically the same oscillator strength and excitation potential of the lower level but differ in the effective Lande factor.
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