Titlebook: Compact Stars; Nuclear Physics, Par Norman K. Glendenning Textbook 19971st edition Springer-Verlag New York, Inc. 1997 Redshift.Variation.b

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https://doi.org/10.1007/978-3-658-26429-1as such a fundamental implication that it should not be overlooked. We will find that the conventional interpretation of pulsars as neutron stars—or any any other type of star that is gravitationally bound—can be ruled out if any pulsar is found to rotate at a frequency above a certain limit.

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0941-7834 f a second, and their magnetic fields drive intense interstellar dynamos, lighting up entire nebulae. This text discusses the physics of these extreme objects. It includes the needed background in classical general relativity in nuclear and particle physics.978-1-4684-0491-3Series ISSN 0941-7834 Ser

engagement

https://doi.org/10.1007/978-3-662-68498-6 centrifugal force. When the core of a massive star collapses to produce a neutron star, conservation of angular momentum assures its enhanced rotation, sometimes rapid. Therefore, in this chapter we are interested in the effects of rotation on the structure and stability of relativistic stars and on spacetime.

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harmony

BET

Bernstein-test

aspect

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,Forschungsanliegen bzw. –thema, it were of infinite extent and neglect the energy associated with boundaries in comparison with the bulk energy. This establishes the frame in which we may work—a Lorentz frame—and the approximation in which we may work—the bulk approximation.

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