A quantum-field theoretical description of superfluid vortex arrays in neutron stars

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dc.contributor.advisor C.A. Engelbrecht and F.A.M. Frescura en_US
dc.contributor.author Kemp, Garreth James
dc.date.accessioned 2012-06-07T11:38:49Z
dc.date.available 2012-06-07T11:38:49Z
dc.date.issued 2012-06-07
dc.date.submitted 2011-10-04
dc.identifier.uri http://hdl.handle.net/10210/5045
dc.description M.Sc. en_US
dc.description.abstract The content of this dissertation is directed at a clearer understanding of pulsar behaviour. Pulsars are neutron stars in relatively early stages of their evolution. The intervals between observed arrival times of pulsar beams have been observed to suddenly decrease implying an increase in the star’s angular velocity Ω. This phenomenon is called a glitch. The first observed glitch occurred in the Vela pulsar (PSR 0833 -45) in 1969. The largest observed glitch also occurred in the Vela pulsar and exhibited a relative spin-up, Ω∕Ω~10−6 [1]. These relative pulsar spin-ups generally fall within the range 10−9 to 10−6 [2]. Pulsar glitches occur as a result of the processes in the interior of a neutron star [3]. Thus, a rigorous study of neutron star interiors is justified. Neutron star interiors are composed of hadronic matter: mostly neutrons, with a few per cent of protons (and, of course, non-hadronic electrons to conserve electric charge). The density of a neutron star interior increases with increasing depth as illustrated in 1.1. en_US
dc.language.iso en en_US
dc.subject Superfluidity en_US
dc.subject Vortex theory (Astrophysics) en_US
dc.subject Neutron stars en_US
dc.subject Pulsars en_US
dc.subject Stellar oscillations en_US
dc.title A quantum-field theoretical description of superfluid vortex arrays in neutron stars en_US
dc.type Thesis en_US

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