The Structure and Evolution of Stars
| Author | : | |
| Rating | : | 4.75 (741 Votes) |
| Asin | : | 1783265809 |
| Format Type | : | paperback |
| Number of Pages | : | 240 Pages |
| Publish Date | : | 2017-03-10 |
| Language | : | English |
DESCRIPTION:
Stars are the fundamental observable constituents of the Universe. The basic equations of a spherical star are derived in detail, the modes of energy transport, the equation of state, the physics of the opacity sources and the nuclear reactions are explained. Readership: Final year undergraduates, first-year PhD students and post-doctoral researchers in the field of astrophysics or astronomy.. They are the first objects we see in the night sky, dominate the light produced in our own and other galaxies and nucleosynthesis in stars produces all the elements heavier than helium. The structure of a star can be described mathematically by differential equations which can be derived from the principles of hydrodynamics, electromagnetic theory, thermodynamics, quantum mechanics, and atomic and nuclear physics. Approximate solutions of the equations for stellar structure are given. The procedure for numerical solution of the equations is outlined. Supernova explosions as the deaths of massive stars along with the nucleosynthesis of elements within stars are explained. A knowledge of stars and their evolution is vital in understanding other astrophysical objects from accreting black holes and galaxies to the Universe itself. The evolution of a star is described from its main sequence evolution through the exhaustion of various nuclear fuels to the end points of evolution such as white dwarfs, neutron stars and black holes. Attention is given to the v
Approximate solutions of the equations for stellar structure are given. The structure of a star can be described mathematically by differential equations which can be derived from the principles of hydrodynamics, electromagnetic theory, thermodynamics, quantum mechanics, and atomic and nuclear physics. The evolution of a star is described from its main sequence evolution through the exhaustion of various nuclear fuels to the end points of evolution such as white dwarfs, neutron stars and black holes. They are the first objects we see in the night sky, dominate the light produced in our own and other galaxies and nucleosynthesis in stars produces all the elements heavier than helium. Attention is given to the virial theorem, polytropic gas spheres and homology principles. The procedure for numerical solution of the equations is outlined. . A knowledge of stars and their evolution is vital in