反向旋转增强2+1维薄壳虫洞的稳定性：线性气体方程视角

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本文探讨了2 + 1维旋转薄壳虫洞（TSW）中的角动量对稳定性的影响，特别关注了当虫洞壳（环）处于反向旋转状态时的现象。作者S.Habib Mazharimousavi和M.Halilsoy从理论物理学的角度出发，研究了这些具有旋转特性的TSWs。他们指出，与正向旋转相比，反向旋转的TSWs在由线性气体状态方程支持的情况下显示出更强的稳定性。这种稳定的特性使得它们对于理解高维虫洞行为提供了有价值的信息。然而，值得注意的是，尽管反向旋转的TSW在静态条件下表现出较高的稳定性，但在受到小的、速度相关的扰动时，其稳定性却会显著下降。这意味着，即使在理想情况下，TSW的稳定性也并非绝对，物理环境中的微小变化可能对其产生影响，促使系统从稳定状态转向不稳定。这在物理学中是重要的发现，因为它揭示了TSW动态行为的复杂性以及外部因素对它们稳定性的重要影响。该研究结果发表在《欧洲物理杂志C》(Eur.Phys.J.C)的一篇文章中，于2014年7月15日接收，9月10日接受，并于9月23日在线发表。作为开放获取的文章，它允许科学家们无障碍地访问和讨论这一前沿的理论成果。对于理解多维度引力理论和宇宙学中的虫洞模型，这篇论文为理论研究者提供了宝贵的参考资料。通过深入研究反向旋转TSW的稳定性，本文为未来探索宇宙结构和量子引力等领域提供了新的视角。

Eur. Phys. J. C (2014) 74:3073

DOI 10.1140/epjc/s10052-014-3073-2

Regular Article - Theoretical Physics

Counter-rotational effects on stability of 2 + 1-dimensional

thin-shell wormholes

S. Habib Mazharimousavi

, M. Halilsoy

Department of Physics, Eastern Mediterranean University, Gazimagusa, Turkey

Received: 15 July 2014 / Accepted: 10 September 2014 / Published online: 23 September 2014

Abstract The role of angular momentum in a 2 + 1-

dimensional rotating thin-shell wormhole (TSW) is consid-

ered. Particular emphasis is given to stability when the shells

(rings) are counter-rotating. We ﬁnd that counter-rotating

halves make the TSW supported by the equation of state

of a linear gas more s table. Under a small velocity dependent

perturbation, however, it becomes unstable.

1 Introduction

Similar to black holes, wormholes in 2 + 1 dimensions also

constitute informative objects to help us learn more about

their higher-dimensional counterparts. The same is also true

for thin-shell wormholes (TSWs) [1] which are constructed

from an energy-momentum at the throat through a cut-and-

paste technique satisfying the proper junction conditions. We

recall that the history of TSWs started with Visser’s construc-

tion in a 3 +1-dimensional ﬂat Minkowski spacetime [1]. At

the same time he extended the idea to the Schwarzschild

spacetime [2]. In his book [3] and work with Poisson [4 ]he

introduced into physics the terminology of TSWs ﬁrst. In the

latter work they considered also the stability of a TSW. Ever

since, there have been extensive attempts to understand the

various features of the new kind of wormholes. For a short list

of such attempts we refer the reader to [5–17] and references

cited therein. Among the works on TSWs we see general-

izations to higher [18–20] and lower [21–23] dimensions,

and extensions to Lovelock gravity [24–27]. The theory has

also been considered in cylindrical symmetry [28–34], dila-

ton theory [35], and so on. The common feature of all these

extensions is that the bulk spacetimes are all static. We are

well aware of the difﬁculties in rotating thin-shell worm-

holes (RTSWs). For this reason we restrict ourselves in this

study to the relatively simpler case of 2 +1 dimensions. The

e-mail: habib.mazhari@emu.edu.tr

e-mail: mustafa.halilsoy@emu.edu.tr

absence of gravitational degrees of freedom, namely, Weyl

curvature in the lower dimension enforces us to add new

physical parameters s uch as cosmological constant, electric /

magnetic charge, scalar charge, and rotation. Our aim in this

study is to consider RTSWs in 2 + 1 dimensions. The met-

ric function contains the square of the angular momentum

, which does not distinguish the cases of ±J for angular

momentum. We recall that rotating TSWs constructed from

a Kerr black hole in 3 + 1 dimensions have been consid-

ered in [36] and their geodesics have been analyzed in [37].

Also rotational effects for collapsing thin shells in 2 +1 and

4 + 1 dimensions have been considered in detail in [38,39],

respectively.

In our analysis of TSWs we observe that the off-diagonal

components of the extrinsic curvature tensor k

and related

components of the surface energy-momentum at the throat

vanish in the case that we assume counter-rotating com-

ponents of shells at the throat. The gas pressures from the

upper and lower shells cancel each other to modify the equa-

tion of state to the extent that it becomes equivalent to a

static case. We may draw a rough analogy with the rotat-

ing Earth. Due to the non-inertial effects curly geodesics of

winds, i.e. the Coriolis effect matching at the equator, are

counter-circular in different hemispheres. If the two hemi-

spheres of our Earth were counter-rotating instead of coro-

tating the curly motions should be identical. Counter-rotation

at the throat in the case of TSWs allows us to choose a simpler

surface energy-momentum tensor and study the stability con-

dition. We can choose, for instance, a linear gas (LG) equation

of state (EoS) at the junction in which the pressure is linearly

related to the mass density. For such a LG the counter-rotating

components make the TSW more stable. Increasing the angu-

lar momentum magnitude, i.e. the relative rotation, stabilizes

the TSW further. Our next attempt toward a s table TSW is

to assume a velocity dependent perturbation of the LG. It is

observed that our stability argument is restricted by the linear

perturbation alone in which at the equilibrium radius (R

)we

have the initial conditions

= 0. Once we assume

123

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