A new solution of embedding class I representing anisotripic fluid sphere in general relativity
Abstract
In the present paper we are willing to model anisotropic star by choosing a new metric potential. All the physical parameters like the matter density, radial and transverse pressure and are regular inside the anisotropic star, with the speed of sound less than the speed of light. So the new solution obtained by us gives satisfactory description of realistic astrophysical compact stars. The model of the present paper is compatible with observational data of compact objects like RX J185637, Her X1, Vela X12 and Cen X3. A particular model of Her X1 (Mass 0.98 and radius=6.7 km.) is studied in detail and found that it satisfies all the condition needed for physically acceptable model. Our model is described analytically as well as with the help of graphical representation.
Received Day Month Year
Revised Day Month Year
Keywords: General relativity, Compact star, Embedding class, anisotropy
PACS numbers: 04.20.q; 04.40.Nr; 04.40.Dg
1 Introduction
To find the exact solution of Einstein field equations is always an interesting topic to the researchers. In 1916 the first exact solution of Einstein field equations for the interior of a compact object was obtained by Schwarzschild and later several relativists obtained new exact solutions. There are a large number of works in literature based on the topic of the exact solutions but very few of them satisfy the required general physical conditions inside the stellar interior. From the analysis of Delgaty & Lake it is well known that out of 127 published solutions only 16 solutions satisfy all the physical conditions. Newton Singh & Pant have given a class of exact solutions of Einstein’s gravitational field equations describing spherically symmetric and static anisotropic stellar type configurations. The solutions were obtained by assuming a particular form of the anisotropy factor. Fodor has proposed an algorithm to generate any number of physically realistic pressure and density profiles for spherical perfect fluid isotropic distributions without evaluating integrals. Mak, Dobson & Harko have derived the upper limits for the massradius ratio for compact general relativistic objects in presence of cosmological constant as well as in presence of a charged distribution . By assuming a particular mass function Sharma & Maharaj found new exact solutions to the Einstein field equations with an anisotropic matter distribution. A distinguishing feature of this class of solutions is that they admit a linear equation of state which can be applied to strange stars with quark matter. Tolman IV solution in the RandallSundrum Braneworld was obtained by Ovalle & Linares . In the context of the RandallSundrum braneworld, the minimal geometric deformation approach (MGD) is used to generate an exact analytic interior solution to fourdimensional effective Einstein’s field equations for a spherically symmetric compact distribution. By using this analytic solution, the authors have developed an exhaustive analysis of the braneworld effects on realistic stellar interiors, finding strong evidences in favor of the hypothesis they have also shown that compactness is reduced due to bulk effects on stellar configurations.
The study of spherically symmetric solution to Einstein equations allow for finding the anisotropy pressures (the radial component of the pressure differs from the angular component)in relativistic astrophysics, which got much attention after the extensive investigations by Bowers & Liang , and the theoretical investigations by Ruderman . Anisotropy of principal pressures can be found when the source is derived from field theories, i.e., when scalar fields are considered as in boson stars , and the role of strange matter with densities higher than neutron stars ( gm/cc).
Local anisotropy in selfgravitating systems were studied by Herrera and Santos and see the the references there in for a review of anisotropic fluid sphere. Anisotropy may occurs in various reasons e.g, the existence of solid core, in presence of type P superfluid, phase transition, rotation, magnetic field, mixture of two fluid, existence of external field etc. To create pressure anisotropy different mechanisms in stellar models have been identified by Ivanov . Durgapal and Bannerji proposed a model of neutron star satisfying all the physical requirements. A good collections of exact solution of Einstein’s field equation can be found in . Li et al. investigated the structure and stability properties of compact astrophysical objects that may be formed from the BoseEinstein condensation of dark matter. They also studied numerically the structure equations of the condensate dark matter stars.
Böhmer and Harko derived upper and lower limits for the basic physical parameters massradius ratio, anisotropy, redshift and total energy for arbitrary anisotropic general relativistic matter distributions in the presence of cosmological constant. They have shown that anisotropic compact stellar type objects can be much more compact than the isotropic ones, and their radii may be close to their corresponding Schwarzschild radii. A new model of anisotropic compact star by assuming Tolman VII gravitational potential for metric has been obtained by Bhar et al. . They obtained an anisotropic compact star of mass , radius 3.8 km. and central density gm/cc. In a recent paper Bhar obtained a model of compact star admitting chaplygin equation of state in FinchSkea spacetime of radius 9.69 km and the mass to be , which is very close to the observational data of the strange star PSR J16142230 reported by Gangopadhyay et al. . Many articles have also discussed on embedding class I solutions that can represent compact stars .
The aim of this paper is to generate a new model of anisotropic relativistic anisotropic star satisfying the Karmakar’s condition. In Section 2, we describe the basic field equations in the form of differential equations governing by the gravitational field and the condition which should satisfy to represent a model of anisotropic compact star of embedding class I. A new model of anisotropic compact star has been obtained in Section 3 by assuming a new form for . The values of the integration constants and are obtained from the matching condition which is given in Section 4. In next section we discuss about the physical analysis of our present model. In the final section we summarize all the obtained results and have shown that the model presented here may relate to various compact stars presented in Table 1 and 2.
2 Interior spacetime and the Einstein Field Equations
The interior of the superdense star is assumed to be described by the line element
(1) 
Where and are functions of the radial coordinate ‘’ only.
Let us assume that the matter within the star is anisotropic in nature and correspondingly the energymomentum tensor is described by,
(2) 
with and , the vector being the fluid 4velocity and is the spacelike vector which is orthogonal to . Here is the matter density, is the the radial and is transverse pressure of the fluid in the orthogonal direction to .
Now for the line element (2) and the matter distribution (2) Einstein Field equations (assuming ) is given by,
(4)  
(5) 
where primes represent differentiation with respect to the radial coordinate . Using Eqs. (4) and (5) we get
(6) 
If the metric given in (2) satisfies the Karmakar’s condition , it will represent an embedding class I spacetime i.e.
(7) 
with , . This condition leads to a differential equation given by
(8) 
On integration we get the relationship between and as
(9) 
where and are constants of integration.
3 A new class of wellbehaved embedding classI solution
To solve the above equation (9), let us assume the metric potential as follows:
(11) 
where is constant having a dimension of length and it will be obtained later from the matching conditions.
4 Matching of interior and exterior spacetime
Assuming the exterior spacetime to be the Schwarzschild exterior solution which is match smoothly with our interior solution and is given by
(17) 
5 Conditions for well behaved solutions
For wellbehaved nature of the solutions for an anisotropic fluid sphere the following conditions should be satisfied:

The solution should be free from physical and geometric singularities, i.e. it should yield finite and positive values of the central pressure, central density and nonzero positive value of and .

The causality condition should be obeyed i.e. velocity of sound should be less than that of light throughout the model. In addition to the above the velocity of sound should be decreasing towards the surface i.e. or and or for i.e. the velocity of sound is increasing with the increase of density and it should be decreasing outwards.

The adiabatic index, for realistic matter should be .

The anisotropy factor should be zero at the center and increasing outward.

For a stable anisotropic compact star, must be satisfied, .
We will check all the conditions one by one in the coming sections.
6 Properties of the new solution
The central pressure and density at the interior is given by
(27)  
(28) 
Plugging and we have obtained central density, surface density and central pressure of some well known stars which is given in Table 2.
To satisfy Zeldovich’s condition at the interior, at center must be . Therefore
(29) 
Now the pressure and density gradients can be written as
(31)  
(32)  
(33) 
where
(34)  
(35)  
(36)  
(37) 
6.1 Energy condition
For physically acceptability our proposed model of compact star should satisfy the null energy condition (NEC), weak energy condition (WEC), strong energy condition (SEC) if the following inequalities hold at every points in the interior of a star.
(38)  
(39)  
(40) 
Due to the complexity of the expression we will take the help of graphical representation. The LHS of the above inequalities are plotted in Fig. 4, which implies that the above energy conditions proposed above are satisfied by our model of compact star.
6.2 Massradius relationship
The mass function of the solution can be determined using the equation given below
(42) 
(43) 
The profile of mass function are shown in Fig. 5. Figure indicates that mass function is a monotonic increasing function of and everywhere within the boundary except at center.
For a model of compact star the ratio of mass to the radius can not be arbitrarily large, it should lie in the range , proposed by Buchdahl . We have also calculated the value of for different compact stars from our model which is shown in Table 1. One can easily check that Buchdahl’s condition is satisfied by our model of compact star.
The surface redshift can be determine by
(44) 
We have also drawn the profile of the surface redshift which is shown in Fig. 5. The Maximum value of the surface redshift of some compact stars are obtained in Table 2. The table shows that the value of the surface redshift , lies in the expected range of Barraco & Hamity .
7 Stability Analysis of the model
7.1 Causality Condition
A model of anisotropic compact star will be physically acceptable if the radial and transverse velocity of sound will be less than 1, known as causality conditions. The radial velocity and transverse velocity of sound can be obtained as
(45) 
The profile of radial and transverse velocity of sound have been plotted in Fig. 6, the profile that our shows that causality condition is satisfied by our model. Using the concept of “cracking” proposed by Herrera to study the stability of anisotropic stars under the radial perturbations, Abreu et al. proved that the region of an anisotropic fluid sphere where is potentially stable but the region is potentially unstable where . From Fig. 7 it is clear that our model is potentially stable. Moreover for an anisotropic model of compact star according to Andréasson . Fig. 7 indicates that cracking method and Andréasson’s condition are verified.
7.2 Stability under three forces acting on the system
We want to examine the stability of our present model under three different forces gravitational force, hydrostatics force and anisotropic force which can be described by the following equation
(46) 
proposed by TolmanOppenheimerVolkov and named as TOV equation.
The quantity represents the gravitational mass within the radius , which can derived from the TolmanWhittaker formula and the Einstein’s field equations and is defined by
(47) 
Plugging the value of in equation (46), we get
(48) 
The above expression may also be written as
(49) 
Here
(50)  
(51)  
(52) 
The three different forces acting on the system are shown in Fig. 8. The figure shows that gravitational force is negative and dominating in nature which is counterbalanced by the combine effect of hydrostatics and anisotropic forces to keep the system in equilibrium.
7.3 Adiabetic Index
For any model of compact star the adiabatic index must be always greater than for static equilibrium according to Heintzmann and Hillebrandt’s concept. The relativistic adiabatic index is given by
(54) 
The profile of are drawn in Fig. 9. The figure shows that everywhere within the fluid sphere.
8 Discussion
Here we have successfully proposed a new model of anisotropic compact star in embedding class I spacetime using a new type of metric potential. In this solution, all the physical quantities are monotonically decreasing outward (Figs. 13, 6) and free from central singularities. Furthermore, the metric potentials, and are increasing function with the increase of radius (Figs. 1, 2, 5, 9). The decreasing nature of pressure and density is again reconfirmed by the negativity of their gradients Fig. 3.
Our presented solution does satisfy the WEC, SEC and NEC (Fig. 4) as well. The stability conditions are satisfied i.e. and (Fig. 7). Therefore, our solution gives us the stable star configuration. Moreover, the TOV equation further supports the stability of the models by counterbalancing all the three forces each other to maintain the hydrostatic equilibrium (Fig. 8). The presented models of the above mentioned compact star candidates fit very well with the observed values of masses and radii. Hence our solution might have astrophysical relevance.
References
 1. M. S. R. Delgaty and K. Lake, Comput. Phys. Commun. 115, 395 (1988).
 2. K. N. Singh, N. Pradhan and N. Pant, Int. J. Theor. Phys. 54, 3408 (2015).
 3. K. N. Singh and N. Pant, Astrophys. Space Sci. 358, 44 (2015).
 4. K. N. Singh and N. Pant, Indian J. Phys. DOI 10.1007/s1264801508154 (2015).
 5. G Fodor grqc/0011040 (2000).
 6. M. K. Mak, P. N. J. Dobson and T. Harko, Mod. Phys. Lett. A 15, 2153 (2000).
 7. M. K. Mak, P. N. J. Dobson and T. Harko, Europhys. Lett. 55, 310 (2001).
 8. R. Sharma and S. D. Maharaj, Mon. Not. R. Astron. Soc. 375, 1265 (2007).
 9. J. Ovalle and F. Linares, Phys. Rev. D 88, 104026 (2013).
 10. R.L. Bowers and E. P. T. Liang, Class. Astrophys. J. 188, 657 (1974).
 11. R. Ruderman, Class. Ann. Rev. Astron. Astrophys. 10, 427 (1972).
 12. F. E. Schunck and E. W. Mielke, Class. Quantum Grav. 20, 301 (2003).
 13. L. Herrera and N. O. Santos, Phys.Report. 286, 53 (1997).
 14. B.V. Ivanov, Phys. Rev. D 65, 104011 (2002).
 15. M. C. Durgapal and R. Bannerji, Astrophys. Space Sci. 84, 409 (1982).
 16. H. Stephani, D. Kramer, M. A. H. MacCallum , C. Hoenselaers and E. Herlt, Exact Solutions of Einsteins Field Equations (Cambridge University Press, Cambridge) 2003.
 17. M. Chaisi and S. D. Maharaj, Gen. Rel. Grav. 37, 1177 (2005).
 18. K. Dev and M. Gleiser, Gen. Rel. Grav. 34, 1793 (2002).
 19. K. Dev and M. Gleiser, Gen. Rel. Grav. 35, 1435 (2003).
 20. L. Herrera, J. Martin and J. Ospino, J. Math. Phys. 43, 4889 (2002).
 21. L. Herrera, A. D. Prisco, J. Martin, J. Ospino, N. O. Santos and O. Troconis, Phys. Rev. D 69, 084026 (2004).
 22. B. V. Ivanov, Phys. Rev. D 65, 10411 (2002).
 23. M. K. Mak and T. Harko, Chin. J. Astron. Astrophys. 2, 248 (2002).
 24. X. Y. Li, T. Harko and K. S. Cheng, J. Cosmo. Astropar. Phys 06, 001 (2012).
 25. C. G. Böhmer and T. Harko, Class. Quant. Grav. 23, 6479 (2006).
 26. P. Bhar, M. Hassan Murad and N. Pant, Astrophys. Space Sci. 359, 13 (2015).
 27. P. Bhar, Astrophys. Space Sci. 359, 41 (2015).
 28. T. Gangopadhyay, S. Ray, X. D. Li, J. Dey and M. Dey, Mon. Not. R. Astron. Soc. 431, 3216 (2013).
 29. K.R. Karmarkar, Proc. Ind. Acad. Sci. A 27, 56 (1948).
 30. S.N. Pandey and S.P. Sharma, Gene. Relativ. Gravit. 14, 113 (1981).
 31. H A Buchdahl, Phys.Rev 116, 1027 (1959).
 32. D.E.Barraco and V.H.Hamity, Phys.Rev.D 65, 124028 (2002).
 33. L. Herrera, Phys. Lett.A 165, 206 (1992).
 34. H. Abreu, H. Hernández, L. A. Núñez, Class. Quantum Gravity 24, 4631 (2007).
 35. H. Andréasson, Commun. Math. Phys. 288, 715 (2009).
 36. H. Heintzmann and W. Hillebrandt, Astron. Astrophys. 38, 51 (1975).
 37. S. K. Maurya, Y. K. Gupta, S. Ray and S. R. Chowdhury, Eur. Phys. J. C 75, 389 (2015).
 38. Y. K. Gupta and J. Kumar, Astrophys. Space Sci. 336, 419 (2011).
 39. S. Kumar and Y. K. Gupta, Int. J. Theor. Phys. 53, 2041 (2014).