We show that if the solar and atmospheric data are both described by maximal vacuum oscillations at the relevant mass scales then there exists a unique mixing matrix for three neutrino flavors. The solution necessarily conserves CP and automatically implies that there is no disappearance of atmospheric νe, consistent with indications from the Super-Kamiokande experiment. We also investigate the...

We report on the changes of the Sun’s subsurface stratification inferred from helioseismology data. Using SOHO/MDI (SOlar and Heliospheric Observatory/Michelson Doppler Imager) data for the last 9 years and, more precisely, the temporal variation of f-mode frequencies, we have computed the variation of the radius of subsurface layers of the Sun by applying helioseismic inversions. We have found...

Neutrino flavor oscillations are currently the most favored way to understand the larger solar B neutrino interaction rate measured by Super-Kamiokande (SK) with respect to the B rate reported by the SNO-collaboration. The SNO rate includes only e-type B neutrinos while SK measures solar neutrinos via neutrino-electron elastic scattering which has a small sensitivity to other (active) flavors a...

On 2008 January 10, the twin Solar Terrestrial Relations Observatory (STEREO) A and B spacecraft conducted a high time cadence study of the solar corona with the Extreme UltraViolet Imager (EUVI) instruments with the aim of investigating coronal dynamics. Observations of the three-dimensional propagation of waves within active region coronal loops and a measurement of the true coronal slow mode...

We show that the use of Doppler shifts of Zeeman sensitive spectral lines to observe waves in sunspots is subject to measurement specific phase shifts arising from, (i) altered height range of spectral line formation and the propagating character of p mode waves in penumbrae, and (ii) Zeeman broadening and splitting. We also show that these phase shifts depend on wave frequencies, strengths and...

Assuming three flavour neutrino mixing takes place in vacuum, we investigate the possibility that the solar νe take part in MSW transitions in the Sun due to ∆m31 ∼ (10 −7 − 10−4) eV 2, followed by long wave length vacuum oscillations on the way to the Earth, triggered by ∆m21 (or ∆m 2 32) ∼ (10−12 − 10−10) eV 2, ∆m31 and ∆m 2 21 (∆m 2 32) being the corresponding neutrino mass squared differenc...

Recent analyses of solar photospheric abundances suggest that the oxygen abundance in the solar atmosphere needs to be revised downwards. In this study we investigate the consequence of this revision on helioseismic analyses of the depth of the solar convection zone and the helium abundance in the solar envelope and find no significant effect. We also find that the revised abundances along with...

We test the relation between relative f -mode frequency variation (δν/ν) and Lagrangian perturbation in the solar radius (δr/r) obtained by Dziembowski & Goode (2004) using several pairs of solar models and show that it doesn’t hold true for any of the model pairs we have used. We attempt to derive a better approximation for the kernel linking the relative frequency changes and the solar radius...

Periodic oscillations are observed in Newton's gravitational constant G that are contemporaneous with length of day data obtained from the International Earth Rotation and Reference System (IERRS). Preliminary research has determined that the oscillatory period of G is ≈ 5.9 years (5.899 ± 0.062 years). In this paper, the oscillations are shown to be concomitant with the Earth's distance from t...

Seismology of stars provides insight into the physical mechanisms taking place in their interior, with modes of oscillation probing different layers. Low-amplitude acoustic oscillations excited by turbulent convection were detected four decades ago in the Sun and more recently in low-mass main-sequence stars. Using data gathered by the Convection Rotation and Planetary Transits mission, we repo...