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Template:Expert-subject In general relativity, a naked singularity is a gravitational singularity without an event horizon. In a black hole, the singularity is completely enclosed by a boundary known as the event horizon, inside which the gravitational force of the singularity is strong enough so that light cannot escape. Hence, objects inside the event horizon—including the singularity itself—cannot be directly observed. A naked singularity, by contrast, is observable from the outside.

The theoretical existence of naked singularities is important because their existence would mean that it would be possible to observe the collapse of an object to infinite density. It would also cause foundational problems for general relativity, because general relativity cannot make predictions about the future evolution of space-time near a singularity. In generic black holes, this is not a problem, as an outside viewer cannot observe the space-time within the event horizon.

Some research has suggested that if loop quantum gravity is correct, then naked singularities could exist in nature, implying that the cosmic censorship hypothesis does not hold. Numerical calculations and some other arguments have also hinted at this possibility.

To this date, no naked singularities (and no event horizons) have been observed.

Predicted formation

From concepts drawn of rotating black holes, it is shown that a singularity, spinning rapidly, can become a ring-shaped object. This results in two event horizons, as well as an ergosphere, which draw closer together as the spin of the singularity increases. When the outer and inner event horizons merge, they shrink toward the rotating singularity and eventually expose it to the rest of the universe.

A singularity rotating fast enough might be created by the collapse of dust or by a supernova of a fast-spinning star. Studies of pulsarsPotter or Ceramic Artist Truman Bedell from Rexton, has interests which include ceramics, best property developers in singapore developers in singapore and scrabble. Was especially enthused after visiting Alejandro de Humboldt National Park. and some computer simulations (Choptuik, 1997) have been performed.

This is an example of a mathematical difficulty (divergence to infinity of the density) which reveals a more profound problem in our understanding of the relevant physics involved in the process. A workable theory of quantum gravity should be able to solve problems such as these.

This model also ignores the relativistic aspects of singularity formation. Such a process involves relativistic effects that cause an asymptotic slowing of time compared to the universe at large. To see a singularity or event horizon form a collapsing mass would have to be observed for far longer than the longest conceivable life-span for a universe like ours. Spinning the collapsing mass in an attempt to create a naked singularity does nothing to get around the relativistic time-dilation observed by the universe that we inhabit. Simply put, while mathematically possible, Template:According to whom.

Metrics

Disappearing event horizons exist in the Kerr metric, which is a spinning black hole in a vacuum. Specifically, if the angular momentum is high enough the event horizons will disappear. Transforming the Kerr metric to Boyer-Lindquist coordinates, it can be shown that the $r$ coordinate (which is not the radius) of the event horizon is

$r_{\pm }=\mu \pm (\mu ^{2}-a^{2})^{1/2}$,

where $\mu =GM/c^{2}$, and $a=J/Mc$. In this case, "event horizons disappear" means when the solutions are complex for $r_{\pm }$, or $\mu ^{2}<a^{2}$.

Disappearing event horizons can also be seen with the Reissner-Nordström geometry of a charged black hole. In this metric it can be shown that the singularities occur at

$r_{\pm }=\mu \pm (\mu ^{2}-q^{2})^{1/2}$,

where $\mu =GM/c^{2}$, and $q=GQ^{2}/(4\pi \epsilon _{0}c^{4})$. Of the three possible cases for the relative values of $\mu$ and $q$, the case where $\mu ^{2}<q^{2}$ causes both $r_{\pm }$ to be complex. This means the metric is regular for all positive values of $r$, or in other words the singularity has no event horizon.

See Kerr-Newman metric for a spinning, charged ring singularity.

Effects

A naked singularity could allow scientists to observe an infinitely dense material, which would under normal circumstances be impossible by the cosmic censorship hypothesis. Without an event horizon of any kind, some speculate that naked singularities could actually emit light.

Cosmic censorship hypothesis

The cosmic censorship hypothesis says that a naked singularity cannot arise in our universe from realistic initial conditions.

In fiction

• M. John Harrison's Kefahuchi Tract trilogy of science fiction novels (Light, Nova Swing and Empty Space) centre upon humanity's exploration of a naked singularity.
• "Dark Peril" by James C. Glass (published in Analog March, 2005), is a story about space travelers on an exploratory mission. While they investigate a strange cosmological phenomenon, their two small space crafts begin to shake, and they are unable to leave the area. One crew member realizes that they are trapped in the Ergosphere of a black hole or naked singularity. The story describes a cluster of multiple black holes or singularities, and what the crew does to try to survive this seemingly inescapable situation.

See also

• Black hole electron
• List of astronomical topics
• List of physics topics

References

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External links

• Naked singularity on arXiv
• M. C. Werner and A. O. Peters, "Magnification relations for Kerr lensing and testing cosmic censorship", Physical Review D, Vol. 76, Issue 6 (2007).
• Pankaj S. Joshi, "Do Naked Singularities Break the Rules of Physics?", Scientific American, January 2009.
• Marcus Chown, "Fast-spinning black holes might reveal all" New Scientist, August 2009.