Exotic bulk viscosity and its influence on neutron star r-modes

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dc.creatorChatterjee, Debarati
dc.creatorBandyopadhyay, Debades
dc.date2006-07-01
dc.date2006-12-27
dc.date.accessioned2026-07-07T10:39:27Z
dc.date.available2026-07-07T10:39:27Z
dc.descriptionWe investigate the effect of exotic matter in particular, hyperon matter on neutron star properties such as equation of state (EoS), mass-radius relationship and bulk viscosity. Here we construct equations of state within the framework of a relativistic field theoretical model. As hyperons are produced abundantly in dense matter, hyperon-hyperon interaction becomes important and is included in this model. Hyperon-hyperon interaction gives rise to a softer EoS which results in a smaller maximum mass neutron star compared with the case without the interaction. Next we compute the coefficient of bulk viscosity and the corresponding damping time scale due to the non-leptonic weak process including $Λ$ hyperons. Further, we investigate the role of the bulk viscosity on gravitational radiation driven r-mode instability in a neutron star of given mass and temperature and find that the instability is effectively suppressed.
dc.description5 pages, 3 figure, presented in the Conference on Isolated Neutron Stars: From the Interior to The Surface, London, UK, 24-28 April, 2006; revised and final version to appear in Astrophys. Space Sci
dc.identifierhttps://arxiv.org/abs/astro-ph/0607005
dc.identifierhttp://arxiv.org/abs/astro-ph/0607005
dc.identifierAstrophys.SpaceSci.308:451-455,2007
dc.identifierdoi:10.1007/s10509-007-9356-4
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/181035
dc.subjectAstrophysics
dc.titleExotic bulk viscosity and its influence on neutron star r-modes
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