›Understanding the Roles of Rotation, Pulsation and Chemical Peculiarities in the Upper Main Sequence

A complex relationship exists between rotation, binarity, pulsation, magnetism and chemical peculiarity in upper main-sequence stars. In the region of the HR-diagram where the classical instability strip crosses the main-sequence, one finds the delta Scuti and gamma Doradus stars, alongside the strongly magnetic roAp stars. Pulsational variability is also observed in evolved stars such as the RR Lyrae and Cepheid stars, as well as the subdwarf and white dwarf stars. Beyond the classical instability strip lie also the slowly pulsating B stars and the beta Cephei variables. Many of the stars in the upper main sequence show chemical peculiarities in their atmospheres which are thought to result from chemical stratification aided by a combination of slow rotation, binarity, and strong magnetic fields; all theories which can be tested with time-resolved photometric and spectroscopic observations. In the era of high-quality and statistically significant samples in Astronomy, we are beginning to understand not only the physical processes that occur in these stars, but also how they interact.

This conference will provide an opportunity for the latest results to be discussed by leading scientists at the forefront of their respective fields. The SOC welcomes applications for contributed talks and posters, and the research talk programme will cover a wide range of topics related to upper part of the HR-diagram including rotation, pulsation and asteroseismology, binarity, activity and magnetism, chemical peculiarity and a balanced programme between observational and theoretical work.