The structure and dynamics of the energy-generating core of the Sun and other stars remain poorly constrained, and poorly understood, in spite of their fundamental role in determining the overall structure and evolution of stars.
The detection of solar normal modes of pressure oscillations (p modes) permitted the development of helioseismology, which has allowed us to accurately describe the internal structure and dynamics of the solar outer radiative and convective zones. The recent tentative detection of buoyancy or gravity modes (g modes) in the Sun as well as the impact of the detection of mixed (p and g) modes in low-mass evolved stars have rejuvenated the quest for understanding the central zone of the stars: the stellar core.
The aim of this series of workshops is to understand the impact of the inferences about the structure and dynamics of stellar cores for solar and stellar evolution, of the solar g-mode detection on spatially resolved inversions of the Sun’s core rotation and subsequently for the detection potential of other data sets of solar and stellar g modes. All of these should have an important, direct impact on our understanding of solar and stellar structure and evolution.