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Vol.2 , No. 2, Publication Date: Jan. 31, 2015, Page: 43-48
type metric potential and a specific choice of pressure anisotropy (∆) which involves a parameterα are obtained. The new solutions are utilized to construct the models for super-dense star models as neutron stars. This class of solutions are well behaved within a wide range of values of the parameter α.In the absence of pressure anisotropy (α=0)present model reduces to the&picture=http://www.aascit.org/aascit/decorators/img/journal/902.jpg)
| [1] | Neeraj Pant, Mathematics Department, National Defence Academy, Khadakwasla, Pune, India. |
| [2] | Narendra Pradhan, Physics Department, National Defence Academy, Khadakwasla, Pune, India. |
| [3] | Mohammad Hassan Murad, Department of Mathematics and Natural Sciences, BRAC University, 66 Mohakhali, Dhaka, Bangladesh. |
| [4] | Manuel Malaver, Department of Basic Sciences, Maritime University of the Caribbean, Catia la Mar, Venezuela. |
In this paper, interior solutions of the Einstein field equations for a anisotropic fluid by considering Hajj-Boutros(1986)type metric potential and a specific choice of pressure anisotropy (∆) which involves a parameterα are obtained. The new solutions are utilized to construct the models for super-dense star models as neutron stars. This class of solutions are well behaved within a wide range of values of the parameter α.In the absence of pressure anisotropy (α=0)present model reduces to the
Keywords
Isotropic Coordinates, Super-Dense Stars, Neutron Stars, Pressure Anisotropy
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