We use a flux transport model to simulate the evolution of the Sun’s magnetic dipole moment, polar fields, and open flux under Maunder minimum conditions. Even when the rate of active region emergence is taken to be a factor of 30 smaller than in recent solar cycles, regular polarity oscillations of the axial dipole and polar fields can be maintained if the speed of the poleward surface flow is...

Available helioseismic data now span almost the entire solar activity cycle 23 making it possible to study solar-cycle related changes of the solar rotation rate in detail. In this paper we study how the solar rotation rate, in particular, the zonal flows change with time. In addition to the zonal flows that show a well known pattern in the solar convection zone, we also study changes in the ra...

Over the past two decades, helioseismology has revolutionized our understanding of the interior structure and dynamics of the Sun. Asteroseismology will soon place this knowledge into a broader context by providing structural data for hundreds of Sun-like stars. Solar-like oscillations have already been detected from the ground in several stars, and NASA’s Kepler mission is poised to unleash a ...

High-cadence multiwavelength optical observations were taken with the Dunn Solar Telescope at the National Solar Observatory, Sacramento Peak, accompanied by Advanced Stokes Polarimeter vector magnetograms. A total of 11 network bright points (NBPs) have been studied at different atmospheric heights using images taken in wave bands centered on Mg i b1 0.4 Å, H , and Ca ii K3. Wavelet analysis w...

Ring-diagram analysis is a technique of local helioseismology used to infer plasma flows in the solar convection zone which generates intermediate data products known as ring-fitting parameters. Knowing the sensitivity of ringfitting parameters to actual flows in the Sun is important for interpreting these measurements.Working in plane-parallel geometry, we compute the linear sensitivity of rin...

We summarize a general formulation of particle propagation in fluctuating media, as applied to the description of neutrino propagation through the sun. It contains the familiar MSW effective hamiltonian, plus corrections which describe neutrino interactions with fluctuations in the medium. An estimate of the size of these corrections for a simple model of solar fluctuations is made, with the co...

where U is the mixing matrix (see Refs. [1–3]). Neutrino oscillations depend on the elements of the mixing matrix U , which determine the amplitude of the oscillations, and on the squared-mass differences ∆m2kj ≡ m 2 k − m 2 j , which determine the oscillation length. The results of solar neutrino experiments (Homestake [4], Kamiokande [5], SAGE [6], GALLEX [7], GNO [8], Super-Kamiokande [9] an...

Solar neutrino oscillations with wavelengths comparable to the Earth-Sun distance provide a viable explanations of the long-standing solar neutrino deecit. They imply a time-dependent modulation of the solar neutrino ux due to the eccentricity of the Earth orbit. Motivated by this testable prediction, we propose a Fourier analysis of the signal observable in real-time, solar neutrino experiment...

Reaction temperature plays a major role in product selectivity in the oscillatory mode of the palladium-catalyzed phenylacetylene oxidative carbonylation reaction. At 40 °C, dimethyl (2Z)-2-phenyl-2-butenedioate is the major product whereas at 0 °C the major product is 5,5-dimethoxy-3-phenyl-2(5H)-furanone. The occurrence of oscillations in pH coincides with an increase in the rate of phenylace...