Understanding the stars is the bedrock of modern astrophysics. Stars are the source of life. The chemical enrichment of our Milky Way and of the Universe withallelementsheavierthanlithiumoriginatesintheinteriorsofstars.Stars arethe tracersofthe dynamics ofthe Universe, gravitationallyimplying much more than meets the eye. Stars ionize the interstellar medium and re-ionized the early intergalactic medium. Understanding stellar structure and evolution is fundamental. While stellar structure and evolution are understood in general terms, we lack important physical ingredients, despite extensive research during recent decades.Classicalspectroscopy, photometry, astrometryandinterferometryof stars have traditionally been used as observational constraints to deduce the internal stellar physics. Unfortunately, these types of observations only allow the tuning of the basic common physics laws under stellar conditions with relatively poor precision. The situation is even more worrisome for unknown aspects of the physics and dynamics in stars. These are usually dealt with by using parameterised descriptions of, e.g., the treatments of convection, rotation, angularmomentumtransport, theequationofstate, atomicdi?usion andsettlingofelements, magneto-hydrodynamicalprocesses, andmore.There is a dearth of observational constraints on these processes, thus solar values areoftenassignedtothem.Yetitishardtoimaginethatonesetofparameters is appropriate for the vast range of stars.This chapter is a journey through the Hertzsprung-Russell (HR) Diagram with stops at all the ellipses shown in Fig. 1.12. We discuss briefly each of the currently known classes of pulsating stars, outlining their most impor- tant properties, suchanbsp;...
|Author||:||C. Aerts, J. Christensen-Dalsgaard, D. W. Kurtz|
|Publisher||:||Springer Science & Business Media - 2010-01-19|