2006/07/31 by Debarati Chatterjee, Debades Bandyopadhyay
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics #Cosmology #Equation of state #Exotic matter #Gamma-ray bursts and supernovae #Gravitational wave #High-pressure geophysics and materials #Hyperon #Instability #Mechanics #Neutron #Neutron star #Nuclear matter #Nuclear physics #Nucleon #Physics #Pulsars and Gravitational Waves Research #RADIUS #Star (game theory) #Thermodynamics #Viscosity #Volume viscosity #astro-ph
paper · pdf · doi:10.1007/s10509-007-9356-4
published as Astrophys.SpaceSci.308:451-455,2007 · 5 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
arxiv created 2006/12/27 · openalex publication_date 2007/03/15 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We 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.