Does the large-scale solar magnetic field distribution really reflect the convective velocity fields?

Solar Physics ◽  
1987 ◽  
Vol 110 (1) ◽  
pp. 51-57 ◽  
Author(s):  
V. Bumba
Keyword(s):  
Magnetic Field ◽  
Field Distribution ◽  
Large Scale ◽  
Solar Magnetic Field ◽  
Velocity Fields ◽  
Magnetic Field Distribution ◽  
Convective Velocity

scholarly journals Large-Scale Solar Magnetic Fields

1976 ◽  
Vol 71 ◽  
pp. 47-67 ◽  
Author(s):  
V. Bumba
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Field Distribution ◽  
Large Scale ◽  
Solar Magnetic Field ◽  
Magnetic Measurements ◽  
Preliminary Investigation ◽  
Longitudinal Distribution ◽  
Solar Magnetic Fields ◽  
Background Fields

The characteristics of the large-scale distribution of the solar magnetic fields on the basis of a series of solar magnetic synoptic charts covering more than 15 years of observations are given. The major part of our information concerns the morphology and only some results deal with the kinematics of the field distribution. Results of averaged solar magnetic field fluxes and polarity reversal studies as well as of preliminary investigation of the very-low angular resolution magnetic measurements are given. The regular zonal and sectoral distribution of photospheric background fields, the different role or visibility of structures in both polarities is discussed. The reflection of both main types of the longitudinal distribution of large-scale solar background magnetic fields (the 27-day, the 28–29-day successions, the ‘supergiant’ structures) in the interplanetary magnetic field distribution is also considered.

RSFP PREDICTIONS FOR TRANSVERSE SOLAR MAGNETIC FIELD DISTRIBUTION FROM SOLAR NEUTRINO DATA

1998 ◽  
Vol 13 (15) ◽  
pp. 1163-1170 ◽  
Author(s):  
B. C. CHAUHAN ◽  
U. C. PANDEY ◽  
S. DEV
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Field Distribution ◽  
Magnetic Moment ◽  
Solar Neutrino ◽  
Solar Magnetic Field ◽  
Magnetic Field Distribution ◽  
The Sun ◽  
Solar Magnetic Fields ◽  
The Magnetic Field

Even though the standard solar model (SSM) has been very successful in predicting the thermal and nuclear evolution of the Sun, it does not throw enough light on solar magnetic activity. In the absence of a generally accepted theory of solar dynamo, various general arguments have been put forth to constrain solar magnetic fields. In the absence of reliable knowledge of solar magnetic fields from available astrophysical data, it may be worthwhile to constrain the solar magnetic fields from solar neutrino observations assuming Resonant Spin-Flavor Precession (RSFP) to be responsible for the solar neutrino deficit. The configuration of solar magnetic field derived in this work is in reasonably good agreement with the magnetic field distribution proposed by Akhmedov et al. (Sov. Phys. JETP68, 250 (1989)). However, the magnetic field distribution in the radiation zone used by Pulido (Phys. Rep.211, 167 (1992)) is ruled out. The magnitude of the magnetic field in the radiation and convective zones of the Sun are very sensitive to the value chosen for the neutrino magnetic moment. However, any change in the value of neutrino magnetic moment does not affect the magnetic field distribution as it only scales the magnetic field strength at different points by the same amount.

Solar magnetic field distribution and geomagnetic activity

1986 ◽  
Vol 30 (2) ◽  
pp. 158-171 ◽  
Author(s):  
Václav Bumba ◽  
Ladislav Hejna ◽  
J. Halenka
Keyword(s):  
Magnetic Field ◽  
Field Distribution ◽  
Geomagnetic Activity ◽  
Solar Magnetic Field ◽  
Magnetic Field Distribution

Magnetic Field Distribution in Aperture of TEM Horn Antenna for Close Proximity RF Immunity Test by Impulsive Excitation Wave

2020 ◽  
Vol 140 (12) ◽  
pp. 601-602
Author(s):  
Gen Kawakami ◽  
Ken Kawamata ◽  
Shinobu Ishigami ◽  
Takeshi Ishida ◽  
Katsushige Harima ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Field Distribution ◽  
Horn Antenna ◽  
Magnetic Field Distribution ◽  
Excitation Wave ◽  
Impulsive Excitation ◽  
Close Proximity ◽  
Tem Horn
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