A new model for spherically symmetric charged compact stars of embedding class one

It is well known that the $V_{n}$, which is $n$ dimensional manifold, can always be embedded in $m[=n(n+1)/2]$ dimensional Pseudo-Euclidean space. In essence $(m-n)[=n(n-1)/2]$ is the minimum extra dimensions of pseudo-Euclidean space which is needed for the embedding class of $V_{n}$. The embedding class turns out to be 6 as the relativistic spacetime is 4 dimensional. The class of general spherical and plane symmetric spacetime are 2 and 3 respectively. The Friedman-Robertson-Lemaître spacetime Friedmann1922 ; Robertson1933 ; Lemaitre1933 is of class 1, but the Schwarzschild exterior and interior solutions are of class 2 and class 1 respectively. Moreover the Kerr metric is of class 5 Kuzeev1980 . However, in the present investigation our discussion is limited to the static spherically symmetric metric in curvature coordinates which is embedable in $5-D$ pseudo Euclidean space and hence is of embedding class one metric.

It is well known that the aforesaid metric is only compatible with two perfect fluid distributions: the first one is the Schwarzschild interior solution Schwarzschild1916 with de Sitter’s and Einstein’s universe as its particular cases, and the second one is the Kohler-Chao solution Kohlar1965 . It is worth to point out that the former one is conformally flat while the latter one is non-conformally flat.

Presently we would like to utilize the embedding class one metric to construct electromagnetic mass models by obtaining charged perfect fluid distributions. Normally when charge can be made zero in a charge fluid distribution, then the subsequent distribution is neutral counterpart of the charged distribution. For example, if we get Schwarzschild’s interior metric after the removal of charge in a charged fluid, then that is called charged analogue of the Schwarzschild interior solution Schwarzschild1916 . On the other hand, if the metric of charged fluid turns out to be flat and also all the physical parameters like pressure, density vanish, the corresponding charged fluid distribution is said to form an electromagnetic mass model, i.e. the entire mass is made up of charge only.

This type of electromagnetic mass model (EMMM) with vanishing charge density was first proposed by Lorentz Lorentz1904 and later on by several other scientists Wheeler1962 ; Feynman1964 ; Florides1974 ; Tiwari1984 ; Gautreau1985 ; Gron1985 ; Gron1986 ; Cooperstock1989 ; Tiwari1991a ; Tiwari1991b ; Tiwari1991c ; Ray1993 ; Ray1997 ; Wilzchek1999 ; Ray2002a ; Ray2002b ; Ray2004a ; Ray2004b ; Ray2006 ; Ray2007b . Unfortunately, in all these electromagnetic mass models the fluid has negative pressure (tension). However, it is true for gaseous spheres though at the boundary the vanishing of the density is not necessary for junction conditions. A model with such a special type of density have been proposed both for the uncharged as well as charged cases Mehra1980 ; Kuchowicz1968 . Another idea about the electromagnetic origin of the electron mass maintains that, due to vacuum polarization, its interior has the equation of state of the kind

where $\rho$ and $p$ represents the density and the pressure respectively. This leads to repulsive pressure and easier junction conditions Florides1974 ; Krori1975 ; Gron1986 ; Cooperstock1989 . It can also be combined with a Weyl-type character of the field Ray1993 . The experimental evidence that the electron’s diameter is not larger than $10^{-16}$ cm leads to the conclusion that the classical model of electron must have a region of negative density Ray1997 .

In this paper we have considered the metric $\nu=n\ln\left(1+{{\it Ar}}^{2}\right)+\ln\left(B\right)$ for $n\geq 2$. The choice of constraint on $n$ is due to the following reasons: (i) for $n=0$, there is no meaning of $\nu$ here in the present context as the spacetime via $\nu$ becomes flat, (ii) for $n=1$, this reduces to the same as the Kohlar-Chao solution Kohlar1965 , and (iii) for $n<2$ the term $(1+Ar^{2})^{(n-2)}$ in the expression of $\lambda$ takes the place in the denominator. We have calculated the data for $n=3.3$ to $1000$ and wanted to see what would happen in the result for very high value of $n$. So, one can look in to the Table 2 that if $n$ be large enough i.e. $n=100$, 1000 and even more then $nA$ becomes approximately a constant, say $nA=C$. This means if we take limit $n$ tends to infinity then the metric $\nu$ will convert to the following form $\nu=C{r}^{2}+\ln~B$, which is the same as metric considered for the solution of EMMM $(\nu=2\,A{r}^{2}+\ln~B)$ Maurya2015a .

In the present work we shall try to form a model for the charged fluid of class one by assuming specific metric potential(s) of the class one metric such that they do not form sub set of the metric potentials of the Kohler-Chao metric Kohlar1965 and the Schwarzschild interior metric (considering de Sitter and Einstein universe) Schwarzschild1916 . Now, if the charge can be made zero in the charged fluid so obtained, the describing metric will turn out to be flat by virtue of the class one structure of the metric.

Outline of the present investigation is as follows: in Sect. 2 the field equations and some specific results are provided under the Einstein-Maxwell spacetime whereas we obtain a new class of solutions in Sect. 3. The matching conditions are discussed in Sect. 4 and physical properties of the model are explored in Sect. 5. We pass some comments in Sect. 6.

To determine the expression for the electric charge, we use the pressure isotropy condition. Therefore, from Eqs. (11) and (12), we get

As a consequence of the above Eq. (14) we conclude that if charge vanishes in a charged fluid of embedding class one then the Schwarzschild interior solution Schwarzschild1916 (or special cases like de Sitter universe or the Einstein universe) or the Kohler-Chao solution Kohlar1965 will be only survived neutral counterpart unless either the survived spacetime metric is flat or the charge cannot be zero. Obviously, in the absence of charge either of two factors on the right hand side of (14) has to be zero. It can be verified that the vanishing of the first factor of (14) gives rise to the Kohlar-Chao solution. However, the vanishing of second factor ultimately provides the Schwarzschild interior solution.

Let us consider that $m(r)$ is the mass function for electrically charged fluid sphere and can be given as

By plugging Eq. (8) and Eq. (14) into Eq. (15), eventually we get

We observe that the expressions for the pressure ($p$), density ($\rho$), electric charge ($q$) and mass ($m$) are dependent on metric function $\nu$. As a consequence we consider the metric function $\nu$ to find the spherically symmetric charged fluid solutions in the following form

where $n$ is a positive number and $A$ is a constant such that $n\geq 2$ and $A>0$.

The above form of the metric potential $\nu(r)$ represents the same $2\Phi(r)$ as considered by Lake Lake2003 in his Eq. (9) for $A=1/\alpha$ and $B=1$. Therefore, the explanations on Eq. (17) are mostly the same as in the Ref. Lake2003 . The function $\nu(r)$ is monotone increasing with a regular minimum at $r=0$. If we look at the mass function $m(r)$ in Eq. (16), then it is clear that by using this source function of Eq. (17), the mass function can easily be evaluated exactly for any $n$. Thus, the metric function $\nu$ will generate a ‘class’ of solutions having the physical properties which are expected to be quite distinct for each value of $n$. It is noted that previously the solutions for either $n=1,...,~5$ Lake1998 or $n\geq 5$ Maurya2011 solutions were known. With $n=1,...,~5$, constitute half of all the previously known physically interesting solutions in curvature coordinates Lake1998 whereas for $N\geq 5$ solutions are acceptable on physical grounds and even exhibit a monotonically decreasing subluminal adiabatic sound speed Maurya2011 . It will be also interesting to note that the above form of $\nu(r)$ is quite different from the function of Schwarzschild or Kohlar-Chao as one can get a hint from Eq. (14). Thus, in the present study we expect that each source function $\nu(r)$ which is a monotone increasing function with a regular minima at $r=0$ necessarily provides, via the mass function in Eq. (16), a static spherically symmetric perfect fluid solution of Einstein’s equations which is regular at $r=0$.

On the other hand, the metric potential $\lambda(r)$ can be obtained from Eq. (8) as

where $n\geq 2$ and $A$, $B$ are positive constants. In Fig. 1 the behaviour of $\nu(r)$ and $\lambda(r)$ are shown.

The expressions of the electromagnetic mass and the electric charge are then given by

where $f=\left(1+A{r}^{2}\right)$, $E={\frac{q}{{r}^{2}}}$ and $D=A\,B\,{n}^{2}K$.

Similarly, the expression for the pressure and the energy density are given by (Fig. 2)

where $p_{1}=[{{2+{A}^{2}{r}^{4}+3\,A{r}^{2}+DA{r}^{2}f^{n}}}]$,  $\rho_{1}=[6-4{A}^{2}{r}^{4}+2A{r}^{2}+DA{{r}^{2}}f^{n}]$.

We suppose that the pressure of the charged fluid sphere is related with the energy density by a parameter $\omega$ as, $p=\omega\,\rho$, which is given by (Fig. 3)

We note from Fig. (3) that the ratio $\omega=p/\rho$ is less than 1 throughout inside the star. This obviously implies that the densities are dominating over the pressures everywhere inside the star and the underlying fluid distribution is non-exotic in nature Rahaman2010 .

The expressions for the pressure gradients (by taking $x=A{r}^{2}$) are given by

where

For any physically acceptable charged solution, the following boundary conditions must be satisfied:

at the surface of charged compact stars, whose mass is same as $M$ at $r=R$.

By matching the first and second fundamental forms, the interior of the metric (2) and the exterior of the metric (32) at the boundary $r=R$ (the Darmois-Israel condition), we can find the constants $D$, $B$ and $M$. These are therefore can be obtained as follows:

where $F=(1+AR^{2})$, $\Psi(R)=1+2n^{2}A^{2}R^{4}+2\,n\,A\,R^{2}\,F$.

However, the value of constant $A$ can be determined by assuming density at the surface of the star i.e. $\rho_{s}$ at $r=R$, so that we get

where $\Omega(R)=[6-4{A}^{2}{R}^{4}+2A{R}^{2}+DA{{R}^{2}}F^{n}]$.

Also the value of constant $K$ can be determined by using the relation $D=A\,B\,{n}^{2}\,K$ as

Let us look at the results so far we have obtained in the previous section. A close observation of the results immediately reveals the following two distinct features:

Let us now, besides the above two general features, try to explore some other physical behaviour of our models.

We have investigated for a new stellar model with spherically symmetric matter distribution under the Einstein-Maxwell spacetime. It is observed that the model represents a compact star of embedding class one. The solutions obtain here are general in their nature having the following two specific features:

(i) The metric becomes flat and also the expressions for the pressure, energy density and electric charge become zero in all the cases if we consider the constant $A=0$, which shows that our solutions represent the so-called ‘electromagnetic mass model’ Lorentz1904 .

(ii) The metric function $\nu(r)$, for the limit $n$ tends to infinity, converts to $\nu(r)=C{r}^{2}+ln~B$, which is the same as considered by Maurya et al. Maurya2015a .

We have also studied several physical aspects of the model and find that all the features are acceptable within the expected demand of the contemporary theoretical works and observational evidences. Some salient features of these physical behaviour of our models are as follows:

(1) Regularity condition: We have discussed the situations in the following cases:

(i) Potentials at the centre $r=0$: From Eqs. (17) and (18), we observe that the metric potentials at the centre $r=0$ becomes $e^{\lambda(0)}=1$ and $e^{\nu(0)}=B$. This implies that metric potentials are singularity free and positive at the centre. However, both are monotonically increasing function (Fig. 1).

(ii) Pressure at the centre $r=0$: From Eq. (21), one can obtain $p_{0}=A\,(2n-D)/8\,\pi$, where $A$ and $D$ are positive. The pressure should be positive at the centre and this implies that $D<2n$.

(iii) Density at the centre $r=0$: From Eq. (22), we get the central density $\rho_{0}=(3\,A\,D/8\,\pi)$ which must be positive at the centre. Since $A$ is positive then $D$ is also positive due to positivity of $\rho$. We know that $D=A\,B\,n^{2}\,K$, where $A$, $B$, $n$ are all positive. This implies that $K$ is also positive.

(2) Casuality and Well behaved condition: The speed of sound as suggested by Canuto Canuto satisfies in the presented compact star model as is evident from Fig. 4.

It can be observed from Fig. 4 that the velocity of sound starts decreasing from $n=3.3$ and this clearly indicates that the solution is well behaved from $n=3.3$ onwards and it seems possible to get a reasonable model even when $n$ tends to infinity.

(3) Energy Conditions: In our model all the energy conditions, viz. NEC, SEC and WEC, satisfy simultaneously at all the interior points of the star.

(4) Generalized TOV equation: The generalized Tolman-Oppenheimer-Volkoff (TOV) equation Tolman1939 ; Oppenheimer1939 satisfies here and indicates that the model is in static equilibrium under the interaction between the gravitational, hydrostatic and electric forces.

(5) Effective mass-radius relation: We have verified that the Buchdahl Buchdahl1959 condition $2M/R<8/9$ satisfies in our model within the stipulated range as can be observed from the Table 4.

(6) Surface red-shift: The surface redshift in the present model is found to be satisfactory as can be seen from Fig. 7.

(7) Electric charge: The amount of charge at the centre and boundary for different stars can be found from Table 5. Fig. 8 depicts that the charge is minimum at the centre and monotonically increasing away from the centre, however it acquires the maximum value at the boundary of the stars.

As a final comment, however, it is to be justified to consider several other aspects of embedding class 1 metric and further investigations on the corresponding model for compact stars as far as ultra-modern observational evidences are concerned.

SKM acknowledges support from the authority of University of Nizwa, Nizwa, Sultanate of Oman. Also SR is thankful to the authority of The Institute of Mathematical Sciences, Chennai, India for providing Associateship under which a part of this work was carried out there.