# Item

ITEM ACTIONSEXPORT

Released

Journal Article

#### Shape of rotating black holes

##### External Resource

No external resources are shared

##### Fulltext (restricted access)

There are currently no full texts shared for your IP range.

##### Fulltext (public)

PRD88_044031.pdf

(Any fulltext), 578KB

##### Supplementary Material (public)

There is no public supplementary material available

##### Citation

Gabach Clement, M. E., & Reiris, M. (2013). Shape of rotating black holes.* Physical Review D,* *88*(4): 044031. doi:10.1103/PhysRevD.88.044031.

Cite as: https://hdl.handle.net/11858/00-001M-0000-0015-13E4-7

##### Abstract

We give a thorough description of the shape of rotating axisymmetric stable black-hole (apparent) horizons applicable in dynamical or stationary regimes. It is found that rotation manifests in the widening of their central regions (rotational thickening), limits their global shapes to the extent that stable holes of a given area A and angular momentum J≠0 form a precompact family (rotational stabilization) and enforces their whole geometry to be close to the extreme-Kerr horizon geometry at almost maximal rotational speed (enforced shaping). The results, which are based on the stability inequality, depend only on A and J. In particular they are entirely independent of the surrounding geometry of the space-time and of the presence of matter satisfying the strong energy condition. A complete set of relations between A, J, the length L of the meridians and the length R of the greatest axisymmetric circle, is given. We also provide concrete estimations for the distance between the geometry of horizons and that of the extreme Kerr, in terms only of A and J. Besides its own interest, the work has applications to the Hoop conjecture as formulated by Gibbons in terms of the Birkhoff invariant, to the Bekenstein-Hod entropy bounds and to the study of the compactness of classes of stationary black-hole space-times.