Anisotropic Fluid Star Model in Isotropic Coordinates

Neeraj Pant; Narendra Pradhan; Manuel Malaver

doi:doi:10.11648/j.ijass.s.2015030101.11

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Anisotropic Fluid Star Model in Isotropic Coordinates

Neeraj Pant, Narendra Pradhan, Manuel Malaver

Published in International Journal of Astrophysics and Space Science (Volume 3, Issue 1-1)

Received: 29 September 2014 Accepted: 5 October 2014 Published: 15 October 2014

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Abstract

We present a spherically symmetric solution of the general relativistic field equations in isotropic coordinates for anisotropic neutral fluid, compatible with a super dense star modeling by considering a specific choice of anisotropy factor  that includes a positive constant “” defined as anisotropy parameter, which varies the relation between the radial and tangential pressure. Further, we have constructed a super-dense star model with all degree of suitability. We have found that the maximum mass decreases with the increase of anisotropy parameter (α). The robustness of our result is that it matches with the recent discoveries.

Published in	International Journal of Astrophysics and Space Science (Volume 3, Issue 1-1) This article belongs to the Special Issue Compact Objects in General Relativity
DOI	10.11648/j.ijass.s.2015030101.11
Page(s)	1-5
Creative Commons	This is an Open Access article, distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution and reproduction in any medium or format, provided the original work is properly cited.
Copyright	Copyright © The Author(s), 2014. Published by Science Publishing Group

Keywords

Isotropic Coordinates, Anisotropic Neutral Fluid, Anisotropy Parameter, Super-Dense Star Model, Radial Pressure, Tangential Pressure

References

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[16]	Malaver, M.: World Applied Programming., 3, 309 (2013).
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APA Style

Neeraj Pant, Narendra Pradhan, Manuel Malaver. (2014). Anisotropic Fluid Star Model in Isotropic Coordinates. International Journal of Astrophysics and Space Science, 3(1-1), 1-5. https://doi.org/10.11648/j.ijass.s.2015030101.11

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ACS Style

Neeraj Pant; Narendra Pradhan; Manuel Malaver. Anisotropic Fluid Star Model in Isotropic Coordinates. Int. J. Astrophys. Space Sci. 2014, 3(1-1), 1-5. doi: 10.11648/j.ijass.s.2015030101.11

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AMA Style

Neeraj Pant, Narendra Pradhan, Manuel Malaver. Anisotropic Fluid Star Model in Isotropic Coordinates. Int J Astrophys Space Sci. 2014;3(1-1):1-5. doi: 10.11648/j.ijass.s.2015030101.11

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@article{10.11648/j.ijass.s.2015030101.11,
  author = {Neeraj Pant and Narendra Pradhan and Manuel Malaver},
  title = {Anisotropic Fluid Star Model in Isotropic Coordinates},
  journal = {International Journal of Astrophysics and Space Science},
  volume = {3},
  number = {1-1},
  pages = {1-5},
  doi = {10.11648/j.ijass.s.2015030101.11},
  url = {https://doi.org/10.11648/j.ijass.s.2015030101.11},
  eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ijass.s.2015030101.11},
  abstract = {We present a spherically symmetric solution of the general relativistic field equations in isotropic coordinates for anisotropic neutral fluid, compatible with a super dense star modeling by considering a specific choice of anisotropy factor  that includes a positive constant “” defined as anisotropy parameter, which varies the relation between the radial and tangential pressure. Further, we have constructed a super-dense star model with all degree of suitability. We have found that the maximum mass decreases with the increase of anisotropy parameter (α). The robustness of our result is that it matches with the recent discoveries.},
 year = {2014}
}

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TY  - JOUR
T1  - Anisotropic Fluid Star Model in Isotropic Coordinates
AU  - Neeraj Pant
AU  - Narendra Pradhan
AU  - Manuel Malaver
Y1  - 2014/10/15
PY  - 2014
N1  - https://doi.org/10.11648/j.ijass.s.2015030101.11
DO  - 10.11648/j.ijass.s.2015030101.11
T2  - International Journal of Astrophysics and Space Science
JF  - International Journal of Astrophysics and Space Science
JO  - International Journal of Astrophysics and Space Science
SP  - 1
EP  - 5
PB  - Science Publishing Group
SN  - 2376-7022
UR  - https://doi.org/10.11648/j.ijass.s.2015030101.11
AB  - We present a spherically symmetric solution of the general relativistic field equations in isotropic coordinates for anisotropic neutral fluid, compatible with a super dense star modeling by considering a specific choice of anisotropy factor  that includes a positive constant “” defined as anisotropy parameter, which varies the relation between the radial and tangential pressure. Further, we have constructed a super-dense star model with all degree of suitability. We have found that the maximum mass decreases with the increase of anisotropy parameter (α). The robustness of our result is that it matches with the recent discoveries.
VL  - 3
IS  - 1-1
ER  -

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Author Information

Neeraj Pant

Mathematics Department, National Defence Academy, Khadakwasla, Pune-411023, India
Narendra Pradhan

Physics Department, National Defence Academy, Khadakwasla, Pune-411023, India
Manuel Malaver

Department of Basic Sciences, Maritime University of the Caribbean, Catia la Mar, Venezuela

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APA Style

Neeraj Pant, Narendra Pradhan, Manuel Malaver. (2014). Anisotropic Fluid Star Model in Isotropic Coordinates. International Journal of Astrophysics and Space Science, 3(1-1), 1-5. https://doi.org/10.11648/j.ijass.s.2015030101.11

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ACS Style

Neeraj Pant; Narendra Pradhan; Manuel Malaver. Anisotropic Fluid Star Model in Isotropic Coordinates. Int. J. Astrophys. Space Sci. 2014, 3(1-1), 1-5. doi: 10.11648/j.ijass.s.2015030101.11

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AMA Style

Neeraj Pant, Narendra Pradhan, Manuel Malaver. Anisotropic Fluid Star Model in Isotropic Coordinates. Int J Astrophys Space Sci. 2014;3(1-1):1-5. doi: 10.11648/j.ijass.s.2015030101.11

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@article{10.11648/j.ijass.s.2015030101.11,
  author = {Neeraj Pant and Narendra Pradhan and Manuel Malaver},
  title = {Anisotropic Fluid Star Model in Isotropic Coordinates},
  journal = {International Journal of Astrophysics and Space Science},
  volume = {3},
  number = {1-1},
  pages = {1-5},
  doi = {10.11648/j.ijass.s.2015030101.11},
  url = {https://doi.org/10.11648/j.ijass.s.2015030101.11},
  eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ijass.s.2015030101.11},
  abstract = {We present a spherically symmetric solution of the general relativistic field equations in isotropic coordinates for anisotropic neutral fluid, compatible with a super dense star modeling by considering a specific choice of anisotropy factor  that includes a positive constant “” defined as anisotropy parameter, which varies the relation between the radial and tangential pressure. Further, we have constructed a super-dense star model with all degree of suitability. We have found that the maximum mass decreases with the increase of anisotropy parameter (α). The robustness of our result is that it matches with the recent discoveries.},
 year = {2014}
}

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TY  - JOUR
T1  - Anisotropic Fluid Star Model in Isotropic Coordinates
AU  - Neeraj Pant
AU  - Narendra Pradhan
AU  - Manuel Malaver
Y1  - 2014/10/15
PY  - 2014
N1  - https://doi.org/10.11648/j.ijass.s.2015030101.11
DO  - 10.11648/j.ijass.s.2015030101.11
T2  - International Journal of Astrophysics and Space Science
JF  - International Journal of Astrophysics and Space Science
JO  - International Journal of Astrophysics and Space Science
SP  - 1
EP  - 5
PB  - Science Publishing Group
SN  - 2376-7022
UR  - https://doi.org/10.11648/j.ijass.s.2015030101.11
AB  - We present a spherically symmetric solution of the general relativistic field equations in isotropic coordinates for anisotropic neutral fluid, compatible with a super dense star modeling by considering a specific choice of anisotropy factor  that includes a positive constant “” defined as anisotropy parameter, which varies the relation between the radial and tangential pressure. Further, we have constructed a super-dense star model with all degree of suitability. We have found that the maximum mass decreases with the increase of anisotropy parameter (α). The robustness of our result is that it matches with the recent discoveries.
VL  - 3
IS  - 1-1
ER  -

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