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OBSERVATIONAL CONSTRAINTS ON THE INTERNAL STRUCTURE AND DYNAMICS OF THE VELA PULSAR MARK ABNEY,1, 2 RICHARD I. EPSTEIN,1 AND ANGELA V. OLINTO1, 2
 

Summary: OBSERVATIONAL CONSTRAINTS ON THE INTERNAL STRUCTURE AND DYNAMICS OF THE VELA PULSAR
MARK ABNEY,1, 2 RICHARD I. EPSTEIN,1 AND ANGELA V. OLINTO1, 2
Received 1996 February 27; accepted 1996 May 20
ABSTRACT
We show that the short spin-up time observed for the Vela pulsar during the 1988 "Christmas" glitch implies
that the coupling time of the pulsar core to its crust is less than 110 s. Ekman pumping cannot explain the fast
core-crust coupling and a more effective coupling is necessary. The internal magnetic field of the Vela pulsar can
provide the necessary coupling if the field threads the core with a magnitude that exceeds 1013
G for a normal
interior and 1011
G for a superconducting interior. These lower bounds favor the hypothesis that the interior of
neutron stars contains superfluid neutrons and protons and challenge the notion that pulsar magnetic fields decay
over million year timescales or that magnetic flux is expelled from the core as the star slows.
Subject headings: magnetic fields -- stars: evolution -- stars: interiors -- stars: neutron
1. THE VELA CHRISTMAS GLITCH
Observations of the Vela pulsar during the 1988 December
24 "Christmas" glitch provide a glimpse of the coupling
between the solid crust and the fluid interior of a neutron star.
The phase residuals for this event are shown in Figure 1
(McCulloch et al. 1990). The nearly linear decay in the

  

Source: Abney, Mark - Department of Human Genetics, University of Chicago

 

Collections: Computer Technologies and Information Sciences; Biology and Medicine