Comparison of the sector and conventional spherical harmonic analyses of the solar magnetic field on the photosphere, source surface, and in the Earth’s orbit on July 10–20, 2004

AbstractSome key physical processes that impact the evolution of Earth's atmosphere on time-scale from days to millennia, such as the EUV emissions, are determined by the solar magnetic field. However, observations of the solar spectral irradiance are restricted to the last few solar cycles and are subject to large uncertainties. We present a physics-based model to reconstruct short-term solar spectral irradiance (SSI) variability. The coronal magnetic field is estimated to employ the Potential Field Source Surface extrapolation (PFSS) based on observational synoptic charts and magnetic flux transport model. The emission is estimated to employ the CHIANTI atomic database 8.0. The performance of the model is compared to the emission observed by TIMED/SORCE.

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Sector spherical harmonic analysis of the solar magnetic field

Geomagnetism and Aeronomy ◽

10.1134/s0016793213010106 ◽

2013 ◽

Vol 53 (1) ◽

pp. 1-4 ◽

Cited By ~ 4

Author(s):

A. F. Kharshiladze ◽

K. G. Ivanov

Keyword(s):

Magnetic Field ◽

Harmonic Analysis ◽

Spherical Harmonic ◽

Solar Magnetic Field ◽

Spherical Harmonic Analysis

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Evolution of Large-Scale Coronal Structures

International Astronomical Union Colloquium ◽

10.1017/s0252921100024945 ◽

1994 ◽

Vol 144 ◽

pp. 29-33

Author(s):

P. Ambrož

Keyword(s):

Magnetic Field ◽

Field Line ◽

Large Scale ◽

Coronal Magnetic Field ◽

Source Surface ◽

Solar Cycles ◽

Characteristic Relationship ◽

The Magnetic Field ◽

Coronal Structures

AbstractThe large-scale coronal structures observed during the sporadically visible solar eclipses were compared with the numerically extrapolated field-line structures of coronal magnetic field. A characteristic relationship between the observed structures of coronal plasma and the magnetic field line configurations was determined. The long-term evolution of large scale coronal structures inferred from photospheric magnetic observations in the course of 11- and 22-year solar cycles is described.Some known parameters, such as the source surface radius, or coronal rotation rate are discussed and actually interpreted. A relation between the large-scale photospheric magnetic field evolution and the coronal structure rearrangement is demonstrated.

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Influence of Cycle Variations in the Global Solar Magnetic Field on Characteristics of the Interplanetary Plasma

Geomagnetism and Aeronomy ◽

10.1134/s0016793220070063 ◽

2020 ◽

Vol 60 (7) ◽

pp. 948-957

Author(s):

I. A. Bilenko

Keyword(s):

Magnetic Field ◽

Solar Magnetic Field ◽

Interplanetary Plasma

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The Evolution of the Solar Magnetic Field

Proceedings of the International Astronomical Union ◽

10.1017/s1743921314004670 ◽

2012 ◽

Vol 10 (H16) ◽

pp. 86-89 ◽

Cited By ~ 2

Author(s):

J. Todd Hoeksema

Keyword(s):

Magnetic Field ◽

Solar Cycle ◽

Solar Magnetic Field ◽

Coronal Holes ◽

Active Regions ◽

Statistical Characteristics ◽

Field Pattern ◽

Small Scale ◽

Polar Caps ◽

Magnetic Elements

AbstractThe almost stately evolution of the global heliospheric magnetic field pattern during most of the solar cycle belies the intense dynamic interplay of photospheric and coronal flux concentrations on scales both large and small. The statistical characteristics of emerging bipoles and active regions lead to development of systematic magnetic patterns. Diffusion and flows impel features to interact constructively and destructively, and on longer time scales they may help drive the creation of new flux. Peculiar properties of the components in each solar cycle determine the specific details and provide additional clues about their sources. The interactions of complex developing features with the existing global magnetic environment drive impulsive events on all scales. Predominantly new-polarity surges originating in active regions at low latitudes can reach the poles in a year or two. Coronal holes and polar caps composed of short-lived, small-scale magnetic elements can persist for months and years. Advanced models coupled with comprehensive measurements of the visible solar surface, as well as the interior, corona, and heliosphere promise to revolutionize our understanding of the hierarchy we call the solar magnetic field.

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