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Pulsar Observations and Neutron Star Models

Published online by Cambridge University Press:  14 August 2015

Gerhard Börner  and
Jeffrey M. Cohen
Gerhard Börner*
Affiliation:
Laboratory for High Energy Astrophysics, NASA/Goddard Space Flight Center, Greenbelt, Md., U.S.A.
Jeffrey M. Cohen*
Affiliation:
Laboratory for High Energy Astrophysics, NASA/Goddard Space Flight Center, Greenbelt, Md., U.S.A.
*
∗Permanent address: Max-Planck-Institut für Physik und Astrophysik München, Germany and National Academy of Science-NRC Research Associate.
∗∗Permanent address: Physics Department, University of Pennsylvania, Philadelphia, Pennsylvania 19104. National Academy of Science-NRC Senior Research Associate.

Abstract

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Information about the physical parameters of neutron stars is obtained from pulsar observations. The energy balance of the Crab Nebula and the Vela X remnant allows one to derive limits for the masses of the Crab and Vela pulsars. Glitch observations provide further clues on the masses of these two pulsars. The degree of confidence with which one should believe the derived numbers is pointed out. The possibility of observing neutron stars in binary systems as pulsating X-ray sources is discussed. Finally, the importance of observing redshifted gamma ray lines from the surface of neutron stars, and thus directly measuring either individual or statistical properties of these objects, is pointed out.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 53: Physics of Dense Matter , 1974 , pp. 227 - 236
Copyright
Copyright © Reidel 1974 

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