The quest for the solar g modes

Solar gravity modes (or g modes) -- oscillations of the solar interior for which buoyancy acts as the restoring force -- have the potential to provide unprecedented inference on the structure and dynamics of the solar core, inference that is not possible with the well observed acoustic modes (or p modes). The high amplitude of the g-mode eigenfunctions in the core and the evanesence of the modes in the convection zone make the modes particularly sensitive to the physical and dynamical conditions in the core. Owing to the existence of the convection zone, the g modes have very low amplitudes at photospheric levels, which makes the modes extremely hard to detect. In this paper, we review the current state of play regarding attempts to detect g modes. We review the theory of g modes, including theoretical estimation of the g-mode frequencies, amplitudes and damping rates. Then we go on to discuss the techniques that have been used to try to detect g modes. We review results in the literature, and finish by looking to the future, and the potential advances that can be made -- from both data and data-analysis perspectives -- to give unambiguous detections of individual g modes. The review ends by concluding that, at the time of writing, there is indeed a consensus amongst the authors that there is currently no undisputed detection of solar g modes.Comment: 71 pages, 18 figures, accepted by Astronomy and Astrophysics Revie

SOLAR AND SUPERNOVA CONSTRAINTS ON COSMOLOGICALLY INTERESTING NEUTRINOS

The sun and core-collapse supernovae produce neutrino spectra that are sensitive to the effects of masses and mixing. Current results from solar neutrino experiments provide perhaps our best evidence for such new neutrino physics, beyond the standard electroweak model. I discuss this evidence as well as the limited possibilities for more conventional explanations. If the resolution of the solar neutrino problem is νe → νµ oscillations, standard seesaw estimates of mντ suggest a cosmologically interesting third-generation neutrino. I discuss recent nucleosynthesis arguments that lead to an important constraint on this possibility. 1 I

Non-Radial Oscillations

The problem of the adiabatic nonradial oscillations of spherical stars is reviewed and results recalled for a variety of models. The anomalous behavior of the eigenfunctions for highly condensed models is related to the apparent mobile singularities depending on the eigenvalues. Tables of Q-values are provided to facilitate possible applications to variable stars. In the case of the gravity modes, the existence of multiple spectra, some stable (g/plus/ modes) and some unstable (g/-/ modes) if superadiabatic and subadiabatic regions alternate, is discussed. As far as vibrational stability is concerned, a general expression is given for the 'damping coefficient'. Attention is drawn to the possibility for g(plus) modes of becoming vibrationally unstable under the effect of various factors and in various models, including the sun where this was advocated as a possibility of relieving the neutrinos difficulty. Finally, the present status of the most obvious candidates among variable stars for nonradial oscillations, the beta Canis Majoris stars and the rapid blue variables (white dwarfs) is briefly reviewed