Using high-resolution ring analysis (HRRA) we deduce subsurface flows within magnetic active regions and within quiet sun. With this procedure we are capable of measuring flows with a horizontal spatial resolution of 2◦ in heliographic angle (or roughly 20 Mm). From the resulting flow fields we deduce mean inflow rates into active regions, mean circulation speeds around active regions, and prob...

New physics near the TeV scale could modify neutrino-matter interactions or generate a relatively large neutrino magnetic (transition) moment. Both types of effects have been discussed since the 1970’s as alternatives to mass-induced neutrino flavor oscillations. Nowadays, the availability of high-statistics data makes it possible to turn the idea around and ask: How well do the simple mass-ind...

We examine the excitation of oscillations in the magnetic network of the Sun through the footpoint motion of photospheric magnetic flux tubes located in intergranular lanes. The motion is derived from a time series of high-resolution G-band and continuum filtergrams using an object-tracking technique. We model the response of the flux tube to the footpoint motion in terms of the Klein-Gordon eq...

In this paper, we study the oscillation of nonlinear fractional nabla difference equations of the form [Formula: see text]where c and α are constants, [Formula: see text] is the Riemann-Liouville fractional nabla difference operator of order [Formula: see text] is a real number, and [Formula: see text]. Some sufficient conditions for oscillation are established.

We consider a class of second-order Emden-Fowler equations with positive and nonpositve neutral coefficients. By using the Riccati transformation and inequalities, several oscillation and asymptotic results are established. Some examples are given to illustrate the main results.

I present a matched-wave asymptotic analysis of the driving of solar oscillations by a general localised source. The analysis provides a simple mathematical description of the asymmetric peaks in the power spectrum in terms of the relative locations of eigenmodes and troughs in the spectral response. It is suggested that the difference in measured phase function between the modes and the trough...

The umbral regions of sunspots and pores in the solar photosphere are generally dominated by $3$~mHz oscillations, which due to $p$-modes penetrating magnetic region. In these locations, wave power is also significantly reduced with respect quiet Sun. However, here we study a pore where oscillations umbra not only comparable, or even larger than that Sun, but main dominant frequency as expected...

Constraints on the core temperature (T c) of the Sun and on neutrino-oscillation parameters are obtained from the existing solar neutrino data, including the recent GALLEX and Kamiokande III results. (1) A purely astrophysical solution to the solar neutrino problem is strongly disfavored by the data: the best fit in a cooler Sun model requires an 8% reduction in T c , but the χ 2 test rejects t...

The universe has always been object of our fascination. Because the Sun is our nearest star naturally a long time ago it became an object of our extensive observations. Nowadays, investigations of the Sun are carried by means of observations and theoretical modeling. Unfortunately, due to their intrinsic complexity most of theoretical models cannot be solved analytically. As a consequence, we a...

There is not as yet full agreement on the mechanism that causes the rapid damping of the oscillations observed by TRACE in coronal loops. It has been suggested that the variation of the observed values of the damping time as function of the corresponding observed values of the period contains information on the possible damping mechanism. The aim of this Letter is to show that, for resonant abs...