New class of relativistic anisotropic strange star in Vaidya-Tikekar model
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ORIGINAL ARTICLE
New class of relativistic anisotropic strange star in Vaidya-Tikekar model K.B. Goswami1 · A. Saha2 · P.K. Chattopadhyay1
Received: 11 March 2020 / Accepted: 14 August 2020 © Springer Nature B.V. 2020
Abstract A new class of compact cold star with strange matter is obtained in a spheroidal space-time with anisotropic pressure described by Vaidya-Tikekar metric. Considering strange matter equation of state namely p = 13 (ρ − 4B), where B is Bag constant in MIT Bag model, we determine the Mass-Radius relationship for Strange Star in four and higher dimensions using the value of surface density ρs = 4B with the allowed value of B (145 MeV < 1 B 4 < 164.4 MeV or equivalently 57.55 MeV/fm3 < B < 95.11 MeV/fm3 ) with respect to neutron for stable strange matter with zero pressure condition. We found that for a constant B, a limiting value of the radius (b) of the star for which geometrical parameter R is real within the allowed range of B as mentioned above. We further note that in four dimension the compactness (ratio of mass to radius) of the star corresponding to the maximum radius is greater than 0.33 in isotropic case and increases when anisotropy increases. In case of five dimensions, we note that same type of nature with different values of compactness is observed. Causality condition holds good through out the star in this model up to a certain values of radius b for which R is real. The information about Mass-to-Radius ratio leads to the de-
B P.K. Chattopadhyay
[email protected] K.B. Goswami [email protected] A. Saha [email protected]
1
Department of Physics, Coochbehar Panchanan Barma University, Vivekananda Street, Coochbehar 736101, West Bengal, India
2
Department of Physics, Alipurduar College, Alipurduar 736122, West Bengal, India
termination of total mass, radius and other physical parameters of the stellar configuration. Keywords Strange star · Compact star · Bag constant · Anisotropic star · Higher dimension
1 Introduction In recent decades the study of compact astrophysical objects is of key interest in both relativistic astrophysics as well as researches in high energy physics too. The basic aim is to study and predict suitable model for compact objects to explain observed properties of compact objects and their internal composition of matter content. The estimated masses and radii of many compact objects are not in well agreement with standard neutron star models as for example the properties of X-ray pulsar Her X-1, X-ray burster 4U 182030, millisecond pulsar SAX J 1808.4-3658, X-ray sources 4U 1728-34, PSR 0943+10 and RX J185635-3754 are not compatible with the standard neutron star models available. The matter densities of such compact objects are generally above the nuclear matter density. Maximum mass and radius of these objects are both less than those for neutron stars, however their compactification factor (ratio of mass to radius) is higher than that of neutron stars. Another way of classifying compact objects is by considering the compactification
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