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Physics and neutron star interiors
Philosophical Transactions of the Royal Society of London. Series A: Physical and Engineering Sciences, 1992Abstract Conditions in neutron stars are more extreme than almost any encountered on Earth: densities exceed those of atomic nuclei, and matter has a large neutron excess. During the past quarter of a century, the challenge of understanding neutron stars has stimulated physicists to confront conditions far different from those ...
C. J. Pethick, D. G. Ravenhall
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1989
With what we now know about the luminosities, radii, masses, and chemical compositions of stars like the sun, our investigation of their internal structures will reveal to us the conditions that must hold throughout a star’s interior if its luminosity is to be consistent with its known mass and radius. To guide us in this investigation we introduce two
Lloyd Motz, Jefferson Hane Weaver
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With what we now know about the luminosities, radii, masses, and chemical compositions of stars like the sun, our investigation of their internal structures will reveal to us the conditions that must hold throughout a star’s interior if its luminosity is to be consistent with its known mass and radius. To guide us in this investigation we introduce two
Lloyd Motz, Jefferson Hane Weaver
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1924
The first “saucy look” into the fiery regions lying deep below the visible surface of the sun and stars is contained in a paper published by Homer Lane in 1870 “On the Theoretical Temperature of the Sun’’. His theory was further developed by A. Ritter, Lord Kelvin, and others; in particular the masterly work of R. Emden in his book Gas- kugeln has been
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The first “saucy look” into the fiery regions lying deep below the visible surface of the sun and stars is contained in a paper published by Homer Lane in 1870 “On the Theoretical Temperature of the Sun’’. His theory was further developed by A. Ritter, Lord Kelvin, and others; in particular the masterly work of R. Emden in his book Gas- kugeln has been
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Physics of Neutron Star Interiors
2001Microscopic Theory of the Nuclear Equation of State and Neutron Star Structure.- Superfluidity in Neutron Star Matter.- Relativistic Superfluid Models for Rotating Neutron Stars.- The Tensor Virial Method and Its Applications to Self-Gravitating Superfluids.- Neutron Star Crusts.- Kaon Condensation in Neutron Stars.- Phases of QCD at High Baryon ...
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Precession as a probe of the neutron star interior
Astrophysics and Space Science, 2007Strong evidence that some neutron stars precess (nutate) with long periods (∼1 yr) challenges our current understanding of the neutron star interior. I describe how neutron star precession can be used to constrain the state of the interior in a new way.
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Neutron stars interiors: Theory and reality
The European Physical Journal A, 2016There are many fascinating processes in the universe which we observe in more detail thanks to increasingly sophisticated technology. One of the most interesting phenomena is the life cycle of stars, their birth, evolution and death. If the stars are massive enough, they end their lives in a core-collapse supernova explosion, one of the most violent ...
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Magnetohydrodynamics of neutron star interiors
2010The dynamics of the charged particles in the fluid interior of rotating magnetized neutron stars (pulsars) is investigated. It is shown that a magnetohydrodynamic approach is valid under a wide variety of conditions. The small amplitude waves that can propagate in the "charged" fluid are sound waves (period ~< 10⁻⁴ sec), inertial waves (≈ 1 sec) and
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The High Density Interiors of Neutron Stars
1991This talk reviews current understanding of the states of matter in the liquid interior of neutron stars — including nuclear matter, pion and kaon condensation, and normal and strange quark matter — and their effect on neutron star structure and dynamics.
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Environmental analysis of a bio-based coating material for automobile interiors
Journal of Cleaner Production, 2022Inês Rodrigues +2 more
exaly
The Physics of the Interiors of the Main Sequence Stars
1980From now on we shall consider the problem of the internal structure of ‘normal’ stars (those which belong to the main sequence of the HR diagram — about 99% of all stars). However, let us start with a summary of the properties of mechanical equilibrium, valid for all static stars, given by the following Subsection and Equations of Chapter 2.
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