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Advances in Mathematical Physics
Volume 2013 (2013), Article ID 630196, 4 pages
http://dx.doi.org/10.1155/2013/630196
Research Article

Neutron Star Interiors and Topology Change

Department of Mathematics, Milwaukee School of Engineering, Milwaukee, WI 53202-3109, USA

Received 1 January 2013; Revised 8 March 2013; Accepted 11 March 2013

Academic Editor: Emilio Elizalde

Copyright © 2013 Peter K. F. Kuhfittig. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.

Abstract

Quark matter is believed to exist in the center of neutron stars. A combined model consisting of quark matter and ordinary matter is used to show that the extreme conditions existing in the center could result in a topology change, that is, in the formation of wormholes.

1. Introduction

Wormholes are handles or tunnels in the spacetime topology connecting different parts of our universe or of different universes. The meticulous analysis in [1] has shown that such wormholes may be actual physical objects permitting two-way passage.

Also introduced in [1] is the metric for a static spherically symmetric wormhole; namely, where . Here is the shape function and is the redshift function, which must be everywhere finite to prevent an event horizon. For the shape function we must have , where is the radius of the throat of the wormhole and also and to satisfy the flare-out condition [1]. We are using geometrized units where .

While Morris and Thorne concentrated on traversable wormholes suitable for humanoid travelers (and possible construction by an advanced civilization), a more general question is the possible existence of naturally occurring wormholes [2]. It has also been suggested that the extreme conditions inside a massive compact star may result in a topology change [3]. It is proposed in this paper that a neutron star is a candidate for such a topology change as a result of quark matter [47], which is believed to exist at the center of neutron stars [8]. To that end, we will use a two-fluid model consisting of ordinary matter and quark matter based on the MIT bag model [9]. Two cases will be considered: the noninteracting and interacting two-fluid models. (We will concentrate mainly on the former case.) The reason for having two cases is that quark matter is a viable candidate for dark matter [10], albeit under different circumstances, and so is likely to be weakly interacting.

A class of exact solutions of the Einstein-Maxwell field equations describing a wormhole with an anisotropic matter distribution is discussed in [11].

A combined model consisting of neutron-star matter and of a phantom/ghost scalar field yielding a nontrivial topology is discussed in [12]. The model is referred to as a neutron-star-plus-wormhole system.

2. Basic Equations

For our basic equations we follow [13]. The energy momentum tensor of the two-fluid model is given by In (2) and (3), and correspond to the respective energy density and pressure of the baryonic matter, while and correspond to the energy density and pressure of the quark matter. The left-hand sides are the effective energy density and pressure, respectively, of the composition.

The Einstein field equations are listed next [13]: recalling that .

In the MIT bag model, the matter equation of state is given by where is the bag constant, which we take to be 145 MeV/(fm)3 [9, 14]. Since quarks are part of the standard model, we assume that ; hence . For normal matter we use the somewhat idealized equation of state [11]

Since we are assuming the pressure to be isotropic, the conservation equation is [13]

3. Solutions of Basic Equations

As noted in the Introduction, we will concentrate mainly on the noninteracting fluid model. This means that the two fluids, normal matter and quark matter, do not interact. The resulting conservation equations are therefore independent of each other. Using (7) and (8), we have The solutions are where and are integration constants. Equations (4), (5), and (6) now give It becomes apparent that this equation is linear in once it is rewritten in the following form: The integrating factor is leading at once to To write the solution for , we first define , which becomes, after substituting the solutions and , We now have The lower limit is the radius of the throat of the wormhole, as we will see.

As noted in Section 1, the shape function is obtained from , so that We obtain Note especially that , which characterizes the throat of the wormhole.

To study the other requirement, , we start with which leads to Given that , the gradient of the redshift function, is related to the tidal force, one would expect its magnitude to be extremely large. So will indeed be less than unity if the expression inside the brackets in (22) is negative and sufficiently small in absolute value. If this is the case, then the flare-out condition is met; that is, Since it indicates a violation of the weak energy condition, the flare-out condition is the primary prerequisite for the existence of wormholes [1]. (The condition will be checked later.)

Unfortunately, the constants and are also large, so that (22) must be examined more closely.

4. The Gradient of the Redshift Function

To analyze (22), we start with the gradient of [15]: where is the total mass-energy inside the radial distance . (This formula is also used in the derivation of the Tolman-Oppenheimer-Volkoff equation.) In geometrized units we get, for ,

Since we are now concerned with what is going to become the throat at , we need to evaluate and in (11) and (12) to obtain So (22) becomes We already know that and that , so that the numerator is indeed negative. For the purpose of comparison, we will simply assume for now that . Then Disregarding for the time being, suppose that we determine so that exceeds . We obtain which leads to  m. The other term in the denominator, , could be close to zero (since ). However, by simply doubling the value of , we can compensate for the normal-matter term in the numerator, since this term is smaller than the other term. Given that the density of nuclear matter ranges from  kg/m3 to  kg/m3, we may take to be about  kg/m3. So in geometrized units, is in fact larger than and reasonably close to , thereby justifying the assumption .

Remark 1. The assumption yields , leading to a negative numerator in (28). It is conceivable that the bag pressure increases with increasing density, but to reverse the sign, the value would have to be more than doubled for a fixed . More importantly, however, (7) suggests that this increase is likely to be compensated for by a concomitant increase in .

Next, given the enormous density near the center of a neutron star,  m would correspond to a fairly small value for : using again, yields  m, although larger values would be allowed. So the above estimate holds.

Finally, observe that the other factor in the denominator, , is now seen to be very close to unity.

We conclude that . So in the neighborhood of the throat, . To show that this inequality holds away from the throat, recall that is the total mass inside a sphere of radius . Hence Since decreases as increases, is positive but decreasing, so that remains less than unity for .

5. Completing the Wormhole Structure

As we have seen, is the mass inside the radial distance . Since is now the throat of the wormhole, it follows from the definition of throat that the interior is outside the manifold. Although not part of the wormhole spacetime, it still contributes to the gravitational field. This can be compared to a thin-shell wormhole from a Schwarzschild black hole [16]: while not part of the manifold, the black hole generates the gravitational field. This comparison explains why our wormhole requires a minimum throat radius to help produce a sufficiently strong gravitational field.

Since the throat of the wormhole is deep inside the neutron star, it cannot be directly observed. According to [12], however, there may still be observable tell-tale signs: if two neutron stars are connected by a wormhole, they would have identical, or nearly identical, characteristics. An even stronger indication would be any observed variation in the mass of a neutron star.

Remark 2. The quark-matter core, being surrounded by nuclear matter, raises a question regarding the interface region. As noted in the Introduction, quark matter is believed to be weakly interacting. So the most likely result is a drop in the energy density in the neighborhood of the core's surface.

5.1. The Need for Quark Matter

If quark matter is eliminated from the model, then the right-hand side of (13) becomes . As a consequence, the term in (28) is also eliminated. Since and , So the fraction in (28) exceeds in absolute value the following: Although we are now dealing with nuclear matter (), we still have . It is quite evident that for close to zero, the fraction in statement (33) is slightly larger than unity in absolute value; hence is negative, which is absurd. As increases, only decreases further, so that the flare-out condition cannot be met.

It now becomes apparent that our conclusion depends critically on the fact that is a constant: increase the throat size until surpasses . So based on our model, a topology change is possible only if there is a sufficient amount of quark matter in the center. More precisely, the assumption implies that the quark matter has to extend at least to .

5.2. The Interacting Case

We conclude with some brief comments on the interacting case. If the two fluids are assumed to interact, then the conservation equations take on the following forms [13, 17]: The quantity expresses the interaction between the two types of matter and falls off rapidly as . Furthermore, since the interaction is assumed to be relatively weak, is a very small quantity compared to . So in comparing and in the expression for , the presence of the quantity is going to have little effect.

6. Conclusion

Quark matter is believed to exist in the center of neutron stars. The analysis in this paper is therefore based on a two-fluid model comprising ordinary and quark matter with an isotropic matter distribution. It is shown that the extreme conditions may result in a topology change; that is, for certain choices of the matter content in the Einstein field equations, a neutron star could give rise to a wormhole.

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