Impact factor of Chinese Physics C is 3.6 in 2023 Impact factor of Chinese Physics C is 3.6 in 2022 2021 Impact Factor 2.944
Advanced Search
×
近期发现有不法分子冒充我刊与作者联系，借此进行欺诈等不法行为，请广大作者加以鉴别，如遇诈骗行为，请第一时间与我刊编辑部联系确认（《中国物理C》（英文）编辑部电话：010-88235947,010-88236950），并作报警处理。
本刊再次郑重声明：
（1）本刊官方网址为cpc.ihep.ac.cn和https://iopscience.iop.org/journal/1674-1137
（2）本刊采编系统作者中心是投稿的唯一路径，该系统为ScholarOne远程稿件采编系统，仅在本刊投稿网网址（https://mc03.manuscriptcentral.com/cpc）设有登录入口。本刊不接受其他方式的投稿，如打印稿投稿、E-mail信箱投稿等，若以此种方式接收投稿均为假冒。
（3）所有投稿均需经过严格的同行评议、编辑加工后方可发表，本刊不存在所谓的“编辑部内部征稿”。如果有人以“编辑部内部人员”名义帮助作者发稿，并收取发表费用，均为假冒。
                  
《中国物理C》（英文）编辑部
2024年10月30日
Chinese Physics C> 2017, Vol. 41> Issue(1) : 015103 DOI: 10.1088/1674-1137/41/1/015103

Anisotropic compact stars in Karmarkar spacetime

  • 1.

      Department of Physics, National Defence Academy, Khadakwasla, Pune-411023, India

  • 2.

      Department of Mathematics, National Defence Academy, Khadakwasla, Pune, 411023, India

  • 3.

      Department of Mathematics, Faculty of Applied Sciences, Durban University of Technology, Durban, South Africa

  • We present a new class of solutions to the Einstein field equations for an anisotropic matter distribution in which the interior space-time obeys the Karmarkar condition. The necessary and sufficient condition required for a spherically symmetric space-time to be of Class One reduces the gravitational behavior of the model to a single metric function. By assuming a physically viable form for the grr metric potential we obtain an exact solution of the Einstein field equations which is free from any singularities and satisfies all the physical criteria. We use this solution to predict the masses and radii of well-known compact objects such as Cen X-3, PSR J0348+0432, PSR B0943+10 and XTE J1739-285.
      PCAS:
  • 加载中

  • References

    [1] K. Schwarzschild, Math. Phys., 189:(1916a)
    [2] K. Schwarzschild, Math. Phys., 424:(1916b)
    [3] R. L. Bowers, E. P. T. Liang, Astrophys. J., 188:657-665(1974)
    [4] J. D. Bekenstein, Phys. Rev. D, 4:2185-2190(1971)
    [5] S. D. Maharaj, R. Maartens, Gen. Relativ. Gravit., 21:899-905(1989)
    [6] R. Tikekar and K. Jotania, Int. J. Mod. Phys. D, 14:1037-1048(2005)
    [7] M. Esculpi et al, Gen. Relativ. Gravit., 39:633-652(2007)
    [8] P. C. Vaidya, Proc. Ind. Acad. Sci. A, 33:264-276(1951)
    [9] N. O. Santos, Mon. Not. R. Astron. Soc., 216:403-410(1985)
    [10] W. B. Bonnor, A. K. G. de Oliveira, and N. O. Santos, Phys. Rep., 181:269-326(1989)
    [11] R. Sharma and R. Tikekar, Pramana J. of Phys., 79:501-509(2012)
    [12] M. Govender et al, Astrophys. Space Sci., 361:33(2016)
    [13] P. Bhar, Astrophys. Space Sci., 356:309-318(2015)
    [14] P. Bhar, Eur. Phys. J. C, 75:123(2015)
    [15] K. N. Singh and N. Pant, Astrophys. Space Sci., 358:44(2015)
    [16] H. Andreasson, J. Phys.:Conference Series, 189:012001-0120013(2009)
    [17] P. Takisa Mafa, S. Ray, S. D. Maharaj, Astrophys. Space Sci., 350:733(2014)
    [18] S. A. Ngubelanga, S. D. Maharaj, and S. Ray, Astrophys. Space Sci., 357:74(2015)
    [19] M. Govender and S. Thirukkanesh, Astrophys. Space Sci., 358:16-22(2015)
    [20] P. Bhar and F. Rahaman, Euro. Phys. J. C, 75:41(2015)
    [21] F.S.N. Lobo, Class. Quantum Grav., 23:1525(2006)
    [22] F. Rahaman et al, Euro. Phys. J. C, 72:2071(2012)
    [23] F. Rahaman et al, Gen. Relativ. Gravit., 44:107-124(2012)
    [24] P. Bhar, Astrophys. Space Sci., 359:41(2015)
    [25] P. H. Chavanis, T. Harko, Phys. Rev. D, 86:064011(2012)
    [26] T. Harko, Phys. Rev. D, 68:064005(2003)
    [27] N. Dadhich et al, Phys. Rev. D, 88:084024(2013)
    [28] P. S. Joshi and D. Malafarina, Int. J. Mod. Phys. D, 20:2641-2729(2011)
    [29] N. Dadhich et al, Phys.Lett. B, 711:196-198(2012)
    [30] S. Hansraj et al, Eur. Phys. J. C, 75:277(2015)
    [31] S. D. Maharaj et al, Phys. Rev. D, 91:084049(2015)
    [32] N. Dadhich et al, Phys. Rev. D, 93:044072(2016)
    [33] A. Banerjee et al, Euro. Phys. J. C, 76:34(2016)
    [34] K. R. Karmarkar, Proc. Indian. Acad. Sci. A, 27:56-60(1948)
    [35] K. N. Singh and N. Pant, Astrophys. Space Sci., 361:177(2016)
    [36] K. N. Singh et al, Astrophys. Space Sci., 361:173(2016)
    [37] S. Thakadiyil and M. K. Jasim, Int. J. Theor. Phys., 52:3960-3964(2013)
    [38] S.N. Pandey and S. P. Sharma, Gene. Relativ. Gravit., 14:113-115(1981)
    [39] L. Herrera and N. O. Santos, Phys. Rep., 286:53-130(1997)
    [40] J. Ponce de Leon, Gen. Relativ. Gravit., 19:797-807(1987)
    [41] T. D. C. Ash et al, Gen. Relativ. Gravit., 307:357-364(1999)
    [42] J. Antoniadis et al, Science, 340:1233232(2013)
    [43] Y. L. Yue et al, Astrophys. J., 649:L95-L98(2006)
    [44] C. M. Zhang et al, Publ. Astron. Soc. Pac., 119:1108-1113(2007)

  • Access

    加载中

Get Citation
Ksh. Newton Singh, Neeraj Pant and M. Govender. Anisotropic compact stars in Karmarkar spacetime[J]. Chinese Physics C, 2017, 41(1): 015103. doi: 10.1088/1674-1137/41/1/015103
Ksh. Newton Singh, Neeraj Pant and M. Govender. Anisotropic compact stars in Karmarkar spacetime[J]. Chinese Physics C, 2017, 41(1): 015103.  doi: 10.1088/1674-1137/41/1/015103 shu
Milestone
Received: 2016-06-19
Article Metric

Article Views(1717)
PDF Downloads(79)
Cited by(0)
Policy on re-use
To reuse of subscription content published by CPC, the users need to request permission from CPC, unless the content was published under an Open Access license which automatically permits that type of reuse.
通讯作者: 陈斌, bchen63@163.com
  • 1. 

    沈阳化工大学材料科学与工程学院 沈阳 110142

  1. 本站搜索
  2. 百度学术搜索
  3. 万方数据库搜索
  4. CNKI搜索

Email This Article

Title:
Email:

Anisotropic compact stars in Karmarkar spacetime

    Corresponding author: Ksh. Newton Singh, ntnphy@gmail.com
    Corresponding author: Neeraj Pant, ntnphy@gmail.com
    Corresponding author: M. Govender, ntnphy@gmail.com
  • 1.  Department of Physics, National Defence Academy, Khadakwasla, Pune-411023, India
  • 2.  Department of Mathematics, National Defence Academy, Khadakwasla, Pune, 411023, India
  • 3.  Department of Mathematics, Faculty of Applied Sciences, Durban University of Technology, Durban, South Africa
  • Received Date: 2016-06-19
  • Available Online: 2017-01-05

Abstract: We present a new class of solutions to the Einstein field equations for an anisotropic matter distribution in which the interior space-time obeys the Karmarkar condition. The necessary and sufficient condition required for a spherically symmetric space-time to be of Class One reduces the gravitational behavior of the model to a single metric function. By assuming a physically viable form for the grr metric potential we obtain an exact solution of the Einstein field equations which is free from any singularities and satisfies all the physical criteria. We use this solution to predict the masses and radii of well-known compact objects such as Cen X-3, PSR J0348+0432, PSR B0943+10 and XTE J1739-285.

    HTML

Reference (44)

目录

Link
IOPScience
SCOAP3
arXiv
Chinese Physical Society
Journal information
Introduction
Editorial Board
Others
Subscribe
Contact us
QQ: 1307685413
Tel: +86-010-88235947
Fax: +86-010-88233126
E-mail: cpc@ihep.ac.cn

  • CPC Website

  • IOP Website

  • CPC WeChat

Copyright © Institute of High Energy Physics, Chinese Academy of Sciences, 19B Yuquan Road, Beijing 100049, China 京ICP备05002789号-1

Supported by: Beijing Renhe Information Technology Co. Ltd  E-mail: info@rhhz.net

/

DownLoad:  Full-Size Img  PowerPoint
Return
Return