2004
DOI: 10.1086/380480
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Abstract: We discuss bounds on the strength of the magnetic fields that could be buried in the radiative zone of the Sun. The field profiles and decay times are computed for all axisymmetric toroidal ohmic decay eigenmodes with lifetimes exceeding the age of the Sun. The measurements of the solar oblateness yield a bound of P7 MG on the strength of the field. A comparable bound is expected to come from the analysis of the splitting of the solar oscillation frequencies. The theoretical analysis of the double diffusive in… Show more

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Cited by 40 publications
(49 citation statements)
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“…In the first case, the parameter β 0 is determined such that the maximum field strength reaches the amplitude of B 0 = 2.1 MG, which is one of the upper limits given by Friedland & Gruzinov (2004) for the present Sun's radiative core. In the second case, it is obtained such that it reaches the arbitrary value of B 0 = 10 kG.…”
Section: Application To Realistic Stellar Interiorsmentioning
confidence: 99%
“…In the first case, the parameter β 0 is determined such that the maximum field strength reaches the amplitude of B 0 = 2.1 MG, which is one of the upper limits given by Friedland & Gruzinov (2004) for the present Sun's radiative core. In the second case, it is obtained such that it reaches the arbitrary value of B 0 = 10 kG.…”
Section: Application To Realistic Stellar Interiorsmentioning
confidence: 99%
“…Not only neutrinos and antineutrinos of all flavors are emitted, not only are there two mass splittings-''solar'' and ''atmospheric''to worry about [17], but the physics of the transformations is significantly richer. For example, several seconds after the onset of the explosion, the flavor conversion probability is affected by the expanding shock front [18] and the turbulent region behind it [19]. The conversion process in such a ''bumpy,'' stochastic profile is qualitatively different from the adiabatic Mikheyev-Smirnov-Wolfenstein (MSW) effect in the smooth, fixed density profile of the Sun.…”
mentioning
confidence: 99%
“…For example, the corresponding frequency shift for the g 2 3 mode (ν = 222.46 μHz) requires a strong radiative-zone magnetic field, B ≥ 8 MG [6], which exceeds established limits for the central magnetic field. In particular, the flattening by ∼10 −5 at the solar poles imposes the constraint B < 7 MG [13]. This seeming contradiction can be understood if the observed frequency shift of the g 2 3 mode is not due to the magnetic field or rotation, but instead to some interactions with other g-modes with frequencies near the Brunt-V¨ais¨al¨a frequency.…”
Section: Discussionmentioning
confidence: 99%