American Journal of Electromagnetics and Applications

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Compact Stellar Model with Two Different Equations of State

Received: 05 June 2019    Accepted: 15 August 2019    Published: 25 February 2020
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Abstract

We have modelled a neutral non-homogeneous anisotropic stellar compact object with two distinct equations of state in general relativity framework. We have considered the macroscopic features of a general relativistic gravitating compact object. The equation of state is quadratic in the core and linear in the envelope. There is smooth matching between the core, envelope and the vacuum exterior regions. We found the masses, radii and compactness of some compact objects such PSR J1614-2230, PSR J1903+0327, Vela X-1, SMC-X-1, Cen X-3; which are in agreement with previous investigations. The gravitational potentials and the matter variables are well behaved throughout the stellar structure. We present in particular the variation of the radius in the core and the envelope of the star by changing some parameters values. Physical features of the pulsars PSR J1614-2230 are presented in more details. It observed that the radial pressure in the core is higher than the radial pressure in the envelope. The investigation reveals that the model is physically relevant for the study of observed compact stars.

DOI 10.11648/j.ajea.20200801.12
Published in American Journal of Electromagnetics and Applications (Volume 8, Issue 1, June 2020)
Page(s) 12-17
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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), 2024. Published by Science Publishing Group

Keywords

General Relativity, Compact Star, Equation of State

References
[1] E. Witten, Phys. Rev. D 30 272, (1984).
[2] E. Farhi and R. L. Jaffe, Phys. Rev. D 30 2379, (1984).
[3] R. Sharma and S. Mukherjee, Mod. Lett. A 17, 2535, (2002).
[4] B. C. Paul and R. Tikekar, Gravit. Cosmol. 11, 244, (2005).
[5] R. Tikekar and K. Jotania, Gravit. Cosmol. 15, 129, (2009).
[6] M. C. Durgapal and G. L. Gehlot, Phys. Rev. D 1830, 1102, (1969).
[7] M. C. Durgapal and G. L. Gehlot, J. Phys. Rev. A 4, 749, (1971).
[8] R. S. Fuloria, M. C. Durgapal and S. C. Pande, Astrophys. Space Sci. 148, 95, (1988).
[9] R. S. Fuloria, M. C. Durgapal and S. C. Pande, Astrophys. Space Sci. 151, 255, (1989).
[10] P. S. Negi, A. K. Pande and M. C. Durgapal, Gen. Relativ. Gravit. 22, 735, (1989).
[11] P. S. Negi, A. K. Pande and M. C. Durgapal, Astrophys. Space Sci. 167, 41, (1990).
[12] R. Sharma and S. Mukherjee, Mod. Phys. Lett. A 16, 1049, (2001).
[13] R. Tikekar and V. O. Thomas, Pramana – J. Phys. 64, 5, (2005).
[14] V. O. Thomas, B. S. RAtanpal and P. C. Vinodkumar, Int. – J. Mod. Phys. D 14, 85, (2005).
[15] R. Ruderman, Astron. Astrophys. 10, 427, (1972).
[16] R. Sharma and B. S. Ratanpal, Int. J. Mod. Phys. D 13, 1350074, (2013).
[17] L. Herrera and W. Barreto, Phys. Rev. D 88, 084022, (2013).
[18] T. Feroze and A. A. Siddiqui, Gen. Relativ. Gravit. 43, 1025, (2011).
[19] S. D. Maharaj and P. Mafa Takisa, Gen. Relativ. Gravit. 44, 1419, (2012).
[20] P. Mafa Takisa, S. D. Maharaj and S. Ray, Astrophys. Space Sci. 354, 463, (2014).
[21] P. Mafa Takisa and S. D. Maharaj, Astrophys. Space Sci. 343, 569, (2013).
[22] S. Thirukkanesh and F. C. Ragel, Pramana – J. Phys. 81, 275 (2013).
[23] P. Mafa Takisa, S. Ray and S. D. Maharaj, Astrophys. Space Sci. 350, 733, (2014).
[24] R. Sharma and S. D. Maharaj, Mon. Not. R. Astron. Soc. 375, 1265, (2007).
[25] T. Gangopadhyay, S. Ray, X-D. Li, J. Dey and M. Dey, Mon. Not. R. Astron. Soc. 431, 3216, (2013).
[26] H. A. Buchdahl, Phys. Rev. 116, 1027, (1959).
[27] M. Azam, S. A. Mardam and M. A. Rehman, Astrophys. Space Sci. 359, 14, (2015).
Author Information
  • Department of Physics, Faculty of Science, University of Kinshasa, Kinshasa, Democratic Republic of Congo

  • Department of Mathematics and Computer Science, Faculty of Science, University of Kinshasa, Kinshasa, Democratic Republic of Congo

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  • APA Style

    Daddy Balondo Iyela, Nestor Anzola Kibamba. (2020). Compact Stellar Model with Two Different Equations of State. American Journal of Electromagnetics and Applications, 8(1), 12-17. https://doi.org/10.11648/j.ajea.20200801.12

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    Daddy Balondo Iyela; Nestor Anzola Kibamba. Compact Stellar Model with Two Different Equations of State. Am. J. Electromagn. Appl. 2020, 8(1), 12-17. doi: 10.11648/j.ajea.20200801.12

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    AMA Style

    Daddy Balondo Iyela, Nestor Anzola Kibamba. Compact Stellar Model with Two Different Equations of State. Am J Electromagn Appl. 2020;8(1):12-17. doi: 10.11648/j.ajea.20200801.12

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  • @article{10.11648/j.ajea.20200801.12,
      author = {Daddy Balondo Iyela and Nestor Anzola Kibamba},
      title = {Compact Stellar Model with Two Different Equations of State},
      journal = {American Journal of Electromagnetics and Applications},
      volume = {8},
      number = {1},
      pages = {12-17},
      doi = {10.11648/j.ajea.20200801.12},
      url = {https://doi.org/10.11648/j.ajea.20200801.12},
      eprint = {https://download.sciencepg.com/pdf/10.11648.j.ajea.20200801.12},
      abstract = {We have modelled a neutral non-homogeneous anisotropic stellar compact object with two distinct equations of state in general relativity framework. We have considered the macroscopic features of a general relativistic gravitating compact object. The equation of state is quadratic in the core and linear in the envelope. There is smooth matching between the core, envelope and the vacuum exterior regions. We found the masses, radii and compactness of some compact objects such PSR J1614-2230, PSR J1903+0327, Vela X-1, SMC-X-1, Cen X-3; which are in agreement with previous investigations. The gravitational potentials and the matter variables are well behaved throughout the stellar structure. We present in particular the variation of the radius in the core and the envelope of the star by changing some parameters values. Physical features of the pulsars PSR J1614-2230 are presented in more details. It observed that the radial pressure in the core is higher than the radial pressure in the envelope. The investigation reveals that the model is physically relevant for the study of observed compact stars.},
     year = {2020}
    }
    

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    T1  - Compact Stellar Model with Two Different Equations of State
    AU  - Daddy Balondo Iyela
    AU  - Nestor Anzola Kibamba
    Y1  - 2020/02/25
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    DO  - 10.11648/j.ajea.20200801.12
    T2  - American Journal of Electromagnetics and Applications
    JF  - American Journal of Electromagnetics and Applications
    JO  - American Journal of Electromagnetics and Applications
    SP  - 12
    EP  - 17
    PB  - Science Publishing Group
    SN  - 2376-5984
    UR  - https://doi.org/10.11648/j.ajea.20200801.12
    AB  - We have modelled a neutral non-homogeneous anisotropic stellar compact object with two distinct equations of state in general relativity framework. We have considered the macroscopic features of a general relativistic gravitating compact object. The equation of state is quadratic in the core and linear in the envelope. There is smooth matching between the core, envelope and the vacuum exterior regions. We found the masses, radii and compactness of some compact objects such PSR J1614-2230, PSR J1903+0327, Vela X-1, SMC-X-1, Cen X-3; which are in agreement with previous investigations. The gravitational potentials and the matter variables are well behaved throughout the stellar structure. We present in particular the variation of the radius in the core and the envelope of the star by changing some parameters values. Physical features of the pulsars PSR J1614-2230 are presented in more details. It observed that the radial pressure in the core is higher than the radial pressure in the envelope. The investigation reveals that the model is physically relevant for the study of observed compact stars.
    VL  - 8
    IS  - 1
    ER  - 

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