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The spin evolution of nascent neutron stars

The spin evolution of nascent neutron stars
The spin evolution of nascent neutron stars
The loss of angular momentum owing to unstable r-modes in hot young neutron stars has been proposed as a mechanism for achieving the spin rates inferred for young pulsars. One factor that could have a significant effect on the action of the r-mode instability is fallback of supernova remnant material. The associated accretion torque could potentially counteract any gravitational-wave-induced spin-down, and accretion heating could affect the viscous damping rates and hence the instability. We discuss the effects of various external agents on the r-mode instability scenario within a simple model of supernova fallback on to a hot young magnetized neutron star. We find that the outcome depends strongly on the strength of the magnetic field of the star. Our model is capable of generating spin rates for young neutron stars that accord well with initial spin rates inferred from pulsar observations. The combined action of r-mode instability and fallback appears to cause the spin rates of neutron stars born with very different spin rates to converge, on a time-scale of approximately 1 year. The results suggest that stars with magnetic fields ?1013 G could emit a detectable gravitational wave signal for perhaps several years after the supernova event. Stars with higher fields (magnetars) are unlikely to emit a detectable gravitational wave signal via the r-mode instability. The model also suggests that the r-mode instability could be extremely effective in preventing young neutron stars from going dynamically unstable to the bar-mode.
accretion, accretion discs, gravitation, magnetic fields, waves, stars: neutron
0035-8711
943-951
Watts, Anna L.
8c906b14-9fb9-4f04-9cb3-2aabd6561162
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Watts, Anna L.
8c906b14-9fb9-4f04-9cb3-2aabd6561162
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304

Watts, Anna L. and Andersson, Nils (2002) The spin evolution of nascent neutron stars. Monthly Notices of the Royal Astronomical Society, 333 (4), 943-951. (doi:10.1046/j.1365-8711.2002.05475.x).

Record type: Article

Abstract

The loss of angular momentum owing to unstable r-modes in hot young neutron stars has been proposed as a mechanism for achieving the spin rates inferred for young pulsars. One factor that could have a significant effect on the action of the r-mode instability is fallback of supernova remnant material. The associated accretion torque could potentially counteract any gravitational-wave-induced spin-down, and accretion heating could affect the viscous damping rates and hence the instability. We discuss the effects of various external agents on the r-mode instability scenario within a simple model of supernova fallback on to a hot young magnetized neutron star. We find that the outcome depends strongly on the strength of the magnetic field of the star. Our model is capable of generating spin rates for young neutron stars that accord well with initial spin rates inferred from pulsar observations. The combined action of r-mode instability and fallback appears to cause the spin rates of neutron stars born with very different spin rates to converge, on a time-scale of approximately 1 year. The results suggest that stars with magnetic fields ?1013 G could emit a detectable gravitational wave signal for perhaps several years after the supernova event. Stars with higher fields (magnetars) are unlikely to emit a detectable gravitational wave signal via the r-mode instability. The model also suggests that the r-mode instability could be extremely effective in preventing young neutron stars from going dynamically unstable to the bar-mode.

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More information

Published date: 2002
Keywords: accretion, accretion discs, gravitation, magnetic fields, waves, stars: neutron

Identifiers

Local EPrints ID: 29448
URI: http://eprints.soton.ac.uk/id/eprint/29448
ISSN: 0035-8711
PURE UUID: f9b4a391-b01b-48ad-9c1c-4d96d8339122
ORCID for Nils Andersson: ORCID iD orcid.org/0000-0001-8550-3843

Catalogue record

Date deposited: 11 May 2006
Last modified: 08 Jan 2022 02:48

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Contributors

Author: Anna L. Watts
Author: Nils Andersson ORCID iD

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