If Be solar neutrinos can be observed in real time experiments, then an extended region of ∆m can be probed by a proper analysis of the rapidly changing phase of vacuum oscillations due to the eccentricity of the earth’s orbit about the sun. For the case of maximal vacuum mixing, a kind of Fourier analysis of expected data for one year’s time could uniquely pick out ∆m if it lies in the region ...

This talk summarizes the results of recent calculations of how fluctuations within the solar medium can influence resonant neutrino oscillations within the sun. Although initial calculations pointed to helioseismic waves as possibly producing detectable effects, recent more careful calculations show this not to be true. Those features of fluctuations which maximize their influence on neutrino p...

In this overview of the MACRO experiment we recall the structure of the detector and discuss several physics topics: atmospheric neutrinos and neutrino oscillations, high energy neutrino astronomy, searches for WIMPs and for low energy stellar gravitational collapse neutrinos, stringent upper limits on GUT magnetic monopoles, high energy downgoing muons, primary cosmic ray composition and shado...

A review of the neutrino conversion and oscillations among the two neutrino species (active and sterile) induced by strong twisting magnetic field is presented and implications to neutrinos in neutron star, supernova, the Sun and interstellar galactic media are discussed. The “cross-boundary effect” (CBE) (i.e., a possible conversion of one half of neutrinos of the bunch from active into steril...

Here, we present a study of the phenomena decayless kink oscillations in system active-region (AR) coronal loops. Using high-resolution observations from two different instruments, namely Extreme Ultraviolet Imager (EUI) on board Solar Orbiter and Atmospheric Imaging Assembly (AIA) Dynamics Observatory, follow these AR loops for an hour each three consecutive days. Our results show significantl...

We review techniques for measuring stellar oscillations in solartype stars. Despite great efforts, no unambiguous detections have been made. A new method, based on monitoring the equivalent widths of strong lines, shows promise but is yet to be confirmed. We also discuss several subtleties, such as the need to correct for CCD non-linearities and the importance of data weighting. 1. Why search f...