The Physics of Stars
A. C. Phillips
- English
- ePUB (mobile friendly)
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The Physics of Stars
A. C. Phillips
About This Book
The Physics of Stars, Second Edition, is a concise introduction to the properties of stellar interiors and consequently the structure and evolution of stars. Strongly emphasising the basic physics, simple and uncomplicated theoretical models are used to illustrate clearly the connections between fundamental physics and stellar properties. This text does not intend to be encyclopaedic, rather it tends to focus on the most interesting and important aspects of stellar structure, evolution and nucleosynthesis. In the Second Edition, a new chapter on Helioseismology has been added, along with a list of physical constants and extra student problems. There is also new material on the Hertztsprung-Russell diagram, as well as a general updating of the entire text. It includes numerous problems at the end of each chapter aimed at both testing and extending student's knowledge.
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1
Basic concepts in astrophysics
1.1 BIG BANG NUCLEOSYNTHESIS
A brief history of the universe
- Nanoseconds after the big bang the universe was filled with a gas of fundamental particles: quarks and antiquarks, leptons and antileptons, neutrinos and antineutrinos, and gluons and photons. When the temperature fell below 1014 K, the quarks, antiquarks and gluons disappeared, annihilating and transforming into less massive particles. Fortunately, because the number of quarks slightly exceeded the number of antiquarks, a few quarks were left behind to form the protons and neutrons present in todayâs universe. The heavier leptons and antileptons were also annihilated as the temperature fell.
- In the interval between a millisecond to a second after the big bang the universe consisted of a gas of neutrons and protons, electrons and positrons, neutrinos and antineutrinos, and photons. As the temperature fell, the density of the universe became too low for the neutrinos to interact effectively with matter; this occurred when the temperature was about 1010 K. These non-interacting, decoupled neutrinos now form a universal gas which, because of the expansion of space, has cooled to a temperature of about 2 K. As yet it has not been possible to detect this universal background of neutrinos. Soon after the decoupling of the neutrinos, the annihilation of electronâpositron pairs removed all of the positrons and most of the electrons.
- After 100 seconds, neutrons combined with protons to form light nuclei, ultimately leading to a universe in which approximately 75% of the mass consists of hydrogen and 25% is helium. We shall explain later how these percentages were determined by the ratio of neutrons to protons in the universe when the neutrinos decoupled.
- After 300 000 years the temperature fell to 4000 K, low enough for the formation of stable atoms. Hydrogen and helium nuclei combined with electrons to form neutral hydrogen and helium atoms. As a result, the photons in the universe ceased to interact strongly with matter; in other words, the universe became transparent to electromagnetic radiation. This radiation, freed from interaction with matter at a temperature near 4000 K, has now cooled to a temperature of about 3 K because of the expansion of the space. It is the cosmic microwave background radiation which was first detected by Penzias and Wilson. This radiation is slightly warmer than the as yet undetected neutrino background at 2 K because, unlike neutrinos, photons were warmed by the heat generated by electronâpositron annihilation in the early universe.
- The universe continued to expand and cool until it reached its present lumpy condition with most of the matter assembled in stars, galaxies and clusters of galaxies.
Cosmic time | Temperature | Temperature |
t â 10â4 s | kT â 102 MeV | Quarks form neutrons and protons |
t â 1 s | kT â 1 MeV | Neutrinos decouple |
t â 4 s | kT â 0.5 MeV | Electronâpositron annihilation |
t â 3 min | kT â 0.1 MeV | Helium and other light nuclei formed |
t â 3 Ă 105 years | kT â 0.3 MeV | Atoms formed and photons decouple |