Stability of the solar neutrino flux derived from SAGE data

Kutvitskii, V. A.; Semikoz, V. B.; Sokoloff, D.

doi:10.1134/s1063772909020097

Cited by 3 publications

(2 citation statements)

References 20 publications

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“…Let us consider a time series f n = f (t n ) where the instants of observations t i = nτ . If the length of the time series is sufficient to consider it as a stationary random process then the random quantity g n = Σ n 0 f i is expected to behave as g n = f n + h(n) where f is the mean of the random process f n and h(n) is a function that grows more slowly then n. By plotting g n against n and comparing the results with a linear trend we can check whether the time series is long enough to be consider as a realization of a stationary random process (for applications of this test in solar physics, see Kutvitskii et al, 2009). The test when applied to the record of solar activity that was exploited by Usoskin et al (2009a) to provide a sequence of Grand Minima, demonstrates substantial deviations from [a linear behaviour].…”

Section: Fluctuations In the Solar Governing Parameters And Grand Minimamentioning

confidence: 99%

Sunspot cycles and Grand Minima

Sokoloff¹,

Arlt²,

Moss³

et al. 2009

Proc. IAU

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Abstract. Observational data concerning the long-term history of cyclic solar activity as recorded in sunspot and isotopic data are discussed in the context of solar dynamo theory. In particular, a simple dynamo model based on differential rotation and the mirror asymmetry of convection with random fluctuations of dynamo governing parameters is shown to reproduce some basic features of the solar magnetic activity evolution.

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Section: Fluctuations In the Solar Governing Parameters And Grand Minimamentioning

confidence: 99%

Sunspot cycles and Grand Minima

Sokoloff¹,

Arlt²,

Moss³

et al. 2009

Proc. IAU

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“…The effect of spin flavor oscillations between active and sterile neutrinos with small δm 2 on the solar neutrino fluxes was discussed in Ref. [69]. The implications of the CP phases of the mixing between active and sterile neutrinos in the scenario with small δm 2 to the effective mass of an electron neutrinos were considered in Ref.…”

Section: Spin Flavor Oscillations Between Electron and Sterile Astrop...mentioning

confidence: 99%

Field theory description of neutrino oscillations

Dvornikov¹

2010

Preprint

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We review various field theory approaches to the description of neutrino oscillations in vacuum and external fields. First we discuss a relativistic quantum mechanics based approach which involves the temporal evolution of massive neutrinos. To describe the dynamics of the neutrinos system we use exact solutions of wave equations in presence of an external field. It allows one to exactly take into account both the characteristics of neutrinos and the properties of an external field. In particular, we examine flavor oscillations an vacuum and in background matter as well as spin flavor oscillations in matter under the influence of an external electromagnetic field. Moreover we consider the situation of hypothetical nonstandard neutrino interactions with background fermions. In the case of ultrarelativistic particles we reproduce an effective Hamiltonian which is used in the standard quantum mechanical approach for the description of neutrino oscillations. The corrections to the quantum mechanical Hamiltonian are also discussed. Note that within the relativistic quantum mechanics method one can study the evolution of both Dirac and Majorana neutrinos. We also consider several applications of this formalism to the description of oscillations of astrophysical neutrinos emitted by a supernova and compare the behavior of Dirac and Majorana neutrinos. Then we study a spatial evolution of mixed massive neutrinos emitted by classical sources. This method seems to be more realistic since it predicts neutrino oscillations in space. Besides oscillations among different neutrino flavors, we also study transitions between particle and antiparticle states. Finally we use the quantum field theory method, which involves virtual neutrinos propagating between production and detection points, to describe particle-antiparticle transitions of Majorana neutrinos in presence of background matter.

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Chemical composition of the atmospheres of red giants with high space velocities

Pakhomov

2012

Astron. Lett.

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The results of a comparative analysis of the elemental abundances in the atmospheres of 14 red giants with high Galactic space velocities are presented. For almost all of the chemical elements considered, the their abundance trends with metallicity correspond to those constructed for thick-disk dwarfs. In the case of sodium, the main factor affecting the [Na/Fe] abundance in the stellar atmosphere for red giants is the surface gravity that characterizes the degree of development of the convective envelope. The difference between the [Na/Fe] abundances in the atmospheres of thin-and thick-disk red giants has been confirmed.

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Stability of the solar neutrino flux derived from SAGE data

Cited by 3 publications

References 20 publications

Sunspot cycles and Grand Minima

Sunspot cycles and Grand Minima

Field theory description of neutrino oscillations

Chemical composition of the atmospheres of red giants with high space velocities

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