Consequences of twisting solar magnetic fields in solar neutrino experiments

1993 ◽  
Vol 48 (12) ◽  
pp. 5496-5504 ◽  
Author(s):  
A. B. Balantekin ◽  
F. Loreti
Keyword(s):  
Magnetic Fields ◽  
Solar Neutrino ◽  
Solar Magnetic Fields ◽  
Neutrino Experiments

THE STATUS OF THE SOLAR NEUTRINO PROBLEM IN THE RESONANT SPIN-FLAVOR PRECESSION SCENARIO WITH TWISTING SOLAR MAGNETIC FIELDS

2000 ◽  
Vol 15 (22n23) ◽  
pp. 1445-1460 ◽  
Author(s):  
S. DEV ◽  
JYOTI DHAR SHARMA
Keyword(s):  
Magnetic Fields ◽  
Solar Neutrino ◽  
Neutrino Flux ◽  
Convective Zone ◽  
Solar Magnetic Fields ◽  
Detection Rates ◽  
Neutrino Detection ◽  
The Status ◽  
Neutrino Experiments ◽  
The Magnetic Field

Resonant spin-flavor precession scenario with twisting solar magnetic fields has been confronted with the solar neutrino data from various ongoing experiments. In particular, the anticorrelation apparent in the Homestake solar neutrino data has been taken seriously to constrain the twisting profiles of the magnetic field in the convective zone of the Sun. The twisting profiles, thus derived, have been used to calculate the neutrino detection rates for the Homestake, Kamiokande (super-Kamiokande) and the gallium experiments. It is found that the presence of twisting reduces the degree of anticorrelation in all the solar neutrino experiments. However, the anticorrelation in the Homestake experiment is expected to be more pronounced. Moreover, the anticorrelation of solar neutrino flux emerging from the southern solar hemisphere is expected to be stronger than that for the neutrinos emerging from the northern solar hemisphere.

scholarly journals Solar neutrino problem accounting for self-consistent magnetohydrodynamics solution for solar magnetic fields

2001 ◽  
Vol 95 (1-3) ◽  
pp. 123-129 ◽  
Author(s):  
O.G. Miranda ◽  
C. Peña-Garay ◽  
T.I. Rashba ◽  
V.B. Semikoz ◽  
J.W.F. Valle
Keyword(s):  
Magnetic Fields ◽  
Solar Neutrino ◽  
Solar Magnetic Fields ◽  
Solar Neutrino Problem ◽  
Self Consistent

RSFP CONSTRAINTS ON THE TWISTING PROFILES OF SOLAR MAGNETIC FIELDS FROM THE SOLAR NEUTRINO DATA

1998 ◽  
Vol 13 (40) ◽  
pp. 3201-3211 ◽  
Author(s):  
UMESH CHANDRA PANDEY ◽  
B. C. CHAUHAN ◽  
S. DEV
Keyword(s):  
Magnetic Fields ◽  
Solar Neutrino ◽  
Convective Zone ◽  
The Sun ◽  
Solar Magnetic Fields

Constraints on the possible twisting profiles of the magnetic fields in the convective zone of the Sun have been derived within the framework of the Resonant Spin Flavor Precession (RSFP) scenario in the light of solar neutrino observations.

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.

Resonant spin-flavor precession constraints on the neutrino parameters and the twisting structure of the solar magnetic fields from the solar neutrino data

Pramana ◽  
2003 ◽  
Vol 61 (1) ◽  
pp. 67-83
Author(s):  
S. Dev ◽  
Jyoti Dhar Sharma ◽  
U. C. Pandey ◽  
S. P. Sud ◽  
B. C. Chauhan
Keyword(s):  
Magnetic Fields ◽  
Solar Neutrino ◽  
Solar Magnetic Fields

RESOLUTION OF THE Be/B SOLAR NEUTRINO FLUX ANOMALY IN THE RESONANT SPIN-FLAVOR PRECESSION SCENARIO WITH TWISTING SOLAR MAGNETIC FIELDS

2000 ◽  
Vol 15 (05) ◽  
pp. 351-360
Author(s):  
S. DEV ◽  
JYOTI DHAR SHARMA
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Seasonal Variations ◽  
Solar Neutrino ◽  
Solar Magnetic Field ◽  
Neutrino Flux ◽  
The Other ◽  
Complete Disappearance ◽  
Solar Magnetic Fields ◽  
Solar Neutrino Flux

The Be/B neutrino flux anomaly has been examined within the framework of the resonant spin-flavor precession scenario with twisting solar magnetic fields. It is found that the twist of the toroidal component of the solar magnetic field, leads naturally to a complete disappearance of 7 Be neutrinos emerging from one of the solar hemispheres. However, the 7 Be neutrino flux emerging from the other solar hemisphere with oppositely twisted magnetic field must survive completely. Thus, this scenario predicts seasonal variations of the 7 Be neutrino flux to be observed in the Borexino experiment.

Magnetic Field Spectroheliograms from the San Fernando Observatory

1971 ◽  
Vol 43 ◽  
pp. 329-339 ◽  
Author(s):  
Dale Vrabec
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Spiral Structure ◽  
Longitudinal Component ◽  
Solar Telescope ◽  
Solar Magnetic Fields ◽  
San Fernando ◽  
Field Lines ◽  
The Magnetic Field ◽  
Field Network

Zeeman spectroheliograms of photospheric magnetic fields (longitudinal component) in the CaI 6102.7 Å line are being obtained with the new 61-cm vacuum solar telescope and spectroheliograph, using the Leighton technique. The structure of the magnetic field network appears identical to the bright photospheric network visible in the cores of many Fraunhofer lines and in CN spectroheliograms, with the exception that polarities are distinguished. This supports the evolving concept that solar magnetic fields outside of sunspots exist in small concentrations of essentially vertically oriented field, roughly clumped to form a network imbedded in the otherwise field-free photosphere. A timelapse spectroheliogram movie sequence spanning 6 hr revealed changes in the magnetic fields, including a systematic outward streaming of small magnetic knots of both polarities within annular areas surrounding several sunspots. The photospheric magnetic fields and a series of filtergrams taken at various wavelengths in the Hα profile starting in the far wing are intercompared in an effort to demonstrate that the dark strands of arch filament systems (AFS) and fibrils map magnetic field lines in the chromosphere. An example of an active region in which the magnetic fields assume a distinct spiral structure is presented.

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