English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We present a family of static and evolving spherically symmetric Lorentzianwormhole solutions in N+1 dimensional Einstein gravity. In general, for staticwormholes, we require that at least the radial pressure has a barotropicequation of state of the form $p_r=\omega_r \rho$, where the state parameter$\omega_r$ is constant. On the other hand, it is shown that in any dimension $N\geq 3$, with $\phi(r)=\Lambda=0$ and anisotropic barotropic pressure withconstant state parameters, static wormhole configurations are alwaysasymptotically flat spacetimes, while in 2+1 gravity there are not onlyasymptotically flat static wormholes and also more general ones. In this case,the matter sustaining the three-dimensional wormhole may be only a pressurelessfluid. In the case of evolving wormholes with $N \geq 3$, the presence of acosmological constant leads to an expansion or contraction of the wormholeconfigurations: for positive cosmological constant we have wormholes whichexpand forever and, for negative cosmological constant we have wormholes whichexpand to a maximum value and then recollapse. In the absence of a cosmologicalconstant the wormhole expands with constant velocity, i.e without accelerationor deceleration. In 2+1 dimensions the expanding wormholes always have anisotropic and homogeneous pressure, depending only on the time coordinate.

N-dimensional static and evolving Lorentzian wormholes with cosmological constant