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Are pulsar glitches triggered by a superfluid two-stream instability?

Are pulsar glitches triggered by a superfluid two-stream instability?
Are pulsar glitches triggered by a superfluid two-stream instability?
Mature neutron stars are expected to have several superfluid components. Strong evidence for this is provided by the glitches that have been observed in dozens of pulsars. The underlying idea behind most glitch models is that, as the neutron star crust spins down due to the emission of electromagnetic radiation, the superfluid component lags behind until a critical point is reached and angular momentum is transferred from the superfluid to the crust, leading to the spin-up associated with the glitch. In this Letter we describe a superfluid analogue of the two-stream instability that is well known in plasma physics, and provide arguments that this instability is likely to be relevant for neutron stars. This is a new physical mechanism which may play a key role in explaining the glitch mechanism and which could also prove to be relevant in laboratory experiments on various superfluid systems.
0031-9007
091101-[4pp]
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Comer, G.L.
f2c1746c-8638-4268-94f0-e5d4375f0358
Prix, R.
96ea3047-4071-44f4-9a9f-e9e331c61421
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Comer, G.L.
f2c1746c-8638-4268-94f0-e5d4375f0358
Prix, R.
96ea3047-4071-44f4-9a9f-e9e331c61421

Andersson, N., Comer, G.L. and Prix, R. (2003) Are pulsar glitches triggered by a superfluid two-stream instability? Physical Review Letters, 90 (9), 091101-[4pp]. (doi:10.1103/PhysRevLett.90.091101).

Record type: Article

Abstract

Mature neutron stars are expected to have several superfluid components. Strong evidence for this is provided by the glitches that have been observed in dozens of pulsars. The underlying idea behind most glitch models is that, as the neutron star crust spins down due to the emission of electromagnetic radiation, the superfluid component lags behind until a critical point is reached and angular momentum is transferred from the superfluid to the crust, leading to the spin-up associated with the glitch. In this Letter we describe a superfluid analogue of the two-stream instability that is well known in plasma physics, and provide arguments that this instability is likely to be relevant for neutron stars. This is a new physical mechanism which may play a key role in explaining the glitch mechanism and which could also prove to be relevant in laboratory experiments on various superfluid systems.

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Published date: March 2003

Identifiers

Local EPrints ID: 29555
URI: http://eprints.soton.ac.uk/id/eprint/29555
ISSN: 0031-9007
PURE UUID: 64a772ce-fcea-4915-876f-8622253f9456
ORCID for N. Andersson: ORCID iD orcid.org/0000-0001-8550-3843

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Date deposited: 12 May 2006
Last modified: 12 Apr 2022 01:35

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Contributors

Author: N. Andersson ORCID iD
Author: G.L. Comer
Author: R. Prix

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