Stars are the fundamental observable constituents of the Universe.
They are the first objects we see in the night sky, they dominate
the light produced in our own and other galaxies, and
nucleosynthesis in stars produces all the elements heavier than
helium. A knowledge of stars and their evolution is vital to
understand other astrophysical objects from accreting black holes
and galaxies to the Universe itself.The structure of a star can be
described mathematically by differential equations derived from the
principles of hydrodynamics, electromagnetic theory,
thermodynamics, quantum mechanics, atomic and nuclear physics. The
basic equations of a spherical star are derived in detail at an
accessible level. The topics discussed include modes of energy
transport, the equation of state, the physics of the opacity
sources and the nuclear reactions. Attention is also given to the
virial theorem, polytropic gas spheres and homology principles and
the procedure for numerical solution of the equations is outlined.
This book tracks the evolution of stars from their main-sequence
evolution through the exhaustion of various nuclear fuels to the
end points of evolution and also introduces the topic of
interacting binary stars. The aim is to take the reader from the
essential underlying physical principles to the doors to current
research on stellar interiors.
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