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The Noise Structure of Pulsar Clocks

Published online by Cambridge University Press:  12 April 2016

Wolfgang Kundt
Wolfgang Kundt*
Affiliation:
Institut für Astrophysik der Universität, Auf dem Hügel 71, D-53121, Bonn

Abstract

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Pulse arrival times of pulsars have a high – though limited – degree of predictability: they show both discrete ‘glitches’, and continuous deviations from an analytic extrapolation of earlier data spans; they are ‘noisy’. This noise shows a strong dependence on a pulsar’s spindown age. Both types of noise can be understood as due to a loose coupling of the charged component of a pulsar’s moment of inertia to a neutral superfluid component, of relative moment of inertia usually below 1%, but reaching 10% in extreme cases. Differential spin rates δΩ/Ω of the two components are ≲ 10−3, usually only ≲ 10−5.

Type
Part 2. Timing, General Relativity and Astrometry
Information
International Astronomical Union Colloquium , Volume 177: Pulsar Astronomy - 2000 and Beyond , 2000 , pp. 103 - 104
Copyright
Copyright © Astronomical Society of the Pacific 2000

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