Gravitational singularity
Imagine a point in the cosmos where the laws of physics as we know them simply... break. That's a gravitational singularity — a theoretical region where gravity becomes so intense that spacetime itself warps infinitely. It's a concept at the heart of black holes and even the very beginning of our universe, yet it pushes the limits of our understanding, hinting at physics beyond our current theories. Gravitational singularities represent extreme points in spacetime where quantities like density and curvature become infinite, signaling the limits of classical general relativity. Black holes famously harbor these singularities, hidden behind an event horizon, where all their mass is compressed into an infinitely small volume. The Big Bang theory also proposes an initial singularity, but a complete understanding of both black hole and cosmic singularities requires a yet-to-be-discovered theory of quantum gravity.
AI Summary
Imagine a point in the cosmos where the laws of physics as we know them simply... break. That's a gravitational singularity — a theoretical region where gravity becomes so intense that spacetime itself warps infinitely. It's a concept at the heart of black holes and even the very beginning of our universe, yet it pushes the limits of our understanding, hinting at physics beyond our current theories.
- Gravitational singularities represent extreme points in spacetime where quantities like density and curvature become infinite, signaling the limits of classical general relativity.
- Black holes famously harbor these singularities, hidden behind an event horizon, where all their mass is compressed into an infinitely small volume.
- The Big Bang theory also proposes an initial singularity, but a complete understanding of both black hole and cosmic singularities requires a yet-to-be-discovered theory of quantum gravity.
What is a Gravitational Singularity?
At its core, a gravitational singularity is a theoretical point in spacetime where the gravitational field is predicted to become infinitely strong. Here, the very fabric of spacetime—the arena in which all events unfold—is thought to break down catastrophically.
For physicists, encountering 'infinities' in equations is often a red flag. It usually signifies that the theory itself is incomplete, much like the ultraviolet catastrophe in classical electromagnetism before quantum mechanics arrived. A singularity suggests a piece of the cosmic puzzle is missing.
In most classical theories, a singularity is a point within a defined spacetime where certain properties become infinite. But in Einstein's General Relativity, it's far more profound. Here, spacetime itself becomes ill-defined, meaning we can't truly say 'where' or 'when' a singularity exists because it's no longer part of the regular spacetime manifold.
Where do Singularities Appear?
The two most famous predictions for gravitational singularities arise from General Relativity: inside black holes and at the very beginning of our universe, during the Big Bang. Both scenarios represent unimaginable extremes of density and gravity.
In black holes, General Relativity predicts that any object collapsing beyond its Schwarzschild radius—a critical point of no return—will inevitably form a singularity. This singularity, however, is shielded from our view by an event horizon, making it forever inaccessible to outside observers.
Our universe's beginning is also theorized to have been a singularity. The Big Bang model suggests that all matter and energy of the observable universe was once compressed into an infinitely dense, infinitely hot point, often referred to as the initial cosmological singularity.
However, classical gravitational theories like General Relativity are not expected to accurately describe such extreme conditions. This is where quantum mechanics steps in, suggesting that perhaps particles cannot occupy a space smaller than their Compton wavelengths, hinting that true infinities might not exist in reality.
Coordinate vs. True Singularities
Not every 'infinity' in a scientific equation points to a true physical singularity. Sometimes, these infinities are merely artifacts of the mathematical coordinate system we choose to describe a region—these are called 'coordinate singularities'.
To determine if a singularity is 'real' or just a mathematical illusion, physicists look for quantities that are 'diffeomorphism invariant.' These are physical properties that remain the same regardless of the coordinate system used. If these invariant quantities, like spacetime curvature, become infinite, then it's a true singularity.
Take the Schwarzschild solution for a non-rotating black hole. In certain coordinate systems, the metric appears to become infinite at the event horizon. Yet, if we switch to a different, more appropriate coordinate system, the spacetime there is perfectly smooth. The true singularity, where invariant curvature does become infinite, lies only at the very center.
One such diffeomorphism invariant quantity is the Kretschmann scalar, which is derived from the Riemann tensor, a mathematical object that quantifies spacetime curvature. If the Kretschmann scalar becomes infinite, you've found a true curvature singularity.
R_{\mu \nu \rho \sigma }R^{\mu \nu \rho \sigma }Shapes and Geometries
Gravitational singularities can come in different theoretical 'shapes.' For a non-rotating, uncharged black hole (like the Schwarzschild solution), the singularity is a single, infinitely dense point—a 'point singularity'.
However, for a rotating black hole, known as a Kerr black hole, the singularity takes on a different form. It's predicted to be stretched out into a ring—a 'ring singularity'—lying in the plane of the black hole's rotation. These are much stranger, theoretically opening up possibilities like wormholes.
Geodesic Incompleteness
Another way to define a singularity is through 'geodesic incompleteness.' A geodesic is the path a freely falling object or light ray takes through spacetime. If such a path abruptly ends after a finite time, without physically reaching anywhere, then spacetime is considered singular.
Consider an observer falling into a non-rotating black hole. Once past the event horizon, their future is sealed. They will inevitably be pulled toward the central singularity within a finite amount of their own proper time, their geodesic terminating abruptly as they are crushed out of existence by infinite tidal forces—a process vividly called 'spaghettification'.
However, this classical picture of a neat, central point singularity can be complicated. Any matter or radiation falling into a black hole would perturb spacetime, causing chaotic oscillations near the singularity, making the final moments of infalling matter even more unpredictable and violent.
For charged or rotating black holes, some theoretical models suggest it might be possible to avoid the singularity. These mathematical extensions hint at pathways through the singularity into different regions of spacetime, possibly even to other universes—though such scenarios are highly unstable and almost certainly destroyed by any real-world perturbation.
Naked Singularities: A Glimpse Beyond?
For decades, it was widely believed that every singularity in our universe must be hidden behind an event horizon, making it impossible for outside observers to witness its chaotic nature. This idea is known as the 'cosmic censorship hypothesis'.
However, in 1991, physicists Stuart Shapiro and Saul Teukolsky conducted computer simulations of collapsing rotating dust that suggested General Relativity might, under certain extreme conditions, allow for 'naked' singularities. These would be singularities exposed directly to the outside universe.
Such 'naked' conditions might theoretically arise in 'extremal black holes'—special cases of rotating or charged black holes where the angular momentum or charge reaches its absolute maximum relative to its mass. At this critical point, the event horizon could, in theory, disappear.
For a Kerr (rotating) black hole, the event horizon radius (r) depends on its mass parameter (µ) and spin parameter (a). If the spin (a) becomes too large relative to the mass (a > µ), the term under the square root becomes negative, leading to complex solutions for r—meaning no real event horizon exists.
r_{\pm } = \mu \pm \left(\mu ^{2}-a^{2}\right)^{1/2}Similarly, for a Reissner-Nordström (charged) black hole, the event horizon depends on mass (µ) and charge (q). If the charge (q) becomes too large compared to the mass (q > µ), the event horizon also vanishes. However, astrophysical black holes are not expected to carry significant net charge.
r_{\pm } = \mu \pm \left(\mu ^{2}-q^{2}\right)^{1/2}What would a naked singularity look like? Nobody knows for certain. Some hypotheses suggest it might still appear like a black hole, as light passing too close would have its path terminated before reaching us. But the possibility of directly observing an exposed singularity remains one of the most exciting and debated ideas in theoretical physics.
Beyond the Singularity: Quantum Gravity's Promise
Ultimately, the existence of gravitational singularities points to a fundamental limitation of General Relativity itself. Many physicists believe that a complete theory of 'quantum gravity,' one that successfully merges General Relativity with quantum mechanics, will resolve these infinities.
The 'fuzzball' model, derived from string theory, proposes that black holes are not empty spacetime leading to a singularity, but rather quantum 'fuzzballs' made of vibrating strings. In this model, there is no singularity or sharp event horizon at all.
Another candidate, Loop Quantum Gravity, also suggests a way around the singularity problem. Instead of infinite density and curvature at the center of a black hole, it posits that these quantities would reach enormous, but finite, maximum values before quantum effects fundamentally alter the fabric of spacetime, preventing a true singularity from forming.
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Gravitational singularity
A gravitational singularity, spacetime singularity, or simply singularity, is a theoretical condition in which gravity is predicted to be so intense that spacetime itself would break down catastrophically. As such, a singularity is by definition no longer part of the regular spacetime and cannot be determined by "where" or "when". Gravitational singularities exist at a junction between general relativity and quantum mechanics; therefore, the properties of the singularity cannot be described without an established theory of quantum gravity. Trying to find a complete and precise definition of singularities in the theory of general relativity, the best theory of gravity available, remains a difficult problem. A singularity in general relativity can be defined by the scalar invariant curvature becoming infinite or, better, by a geodesic being incomplete.
General relativity predicts that any object collapsing beyond its Schwarzschild radius would form a black hole, inside which a singularity will form. A black hole singularity is, however, covered by an event horizon, so it is never in the causal past of any outside observer, and at no time can it be objectively said to have formed. General relativity also predicts that the initial state of the universe, at the beginning of the Big Bang, was a singularity of infinite density and temperature. However, classical gravitational theories are not expected to be accurate under these conditions, and a quantum description is likely needed. For example, quantum mechanics does not permit particles to inhabit a space smaller than their Compton wavelengths.
Interpretation
Gravitational singularity
Many theories in physics have mathematical singularities of one kind or another. Equations for these physical theories predict that the ball of mass of some quantity becomes infinite or increases without limit. This is generally a sign for a missing piece in the theory, as in the ultraviolet catastrophe, re-normalization, and instability of a hydrogen atom predicted by the Larmor formula.
In classical field theories, including special relativity but not general relativity, one can say that a solution has a singularity at a particular point in spacetime where certain physical properties become ill-defined, with spacetime serving as a background field to locate the singularity. A singularity in general relativity, on the other hand, is more complex because spacetime itself becomes ill-defined, and the singularity is no longer part of the regular spacetime manifold. In general relativity, a singularity cannot be defined by "where" or "when".
Some theories, such as the theory of loop quantum gravity, suggest that singularities may not exist. This is also true for such classical unified field theories as the Einstein–Maxwell–Dirac equations. The idea can be stated in the form that, due to quantum gravity effects, there is a minimum distance beyond which the force of gravity no longer continues to increase as the distance between the masses becomes shorter, or alternatively that interpenetrating particle waves mask gravitational effects that would be felt at a distance.
In black holes
Gravitational singularity
Mathematical models of black holes based on general relativities have singularities at their centers—points where the curvature of spacetime becomes infinite, and geodesics terminate within a finite proper time. However, it is unknown whether these singularities truly exist in real black holes. Some physicists believe that singularities do not exist, and that their existence, which would make spacetime unpredictable, signals a breakdown of general relativity and a need for a more complete understanding of quantum gravity. Others believe that such singularities could be resolved within the current framework of physics, without having to introduce quantum gravity. There are also physicists, including Kip Thorne and Charles Misner, who believe that not all singularities can be resolved, and that some likely still exist in the real universe despite the effects of quantum gravity. Finally, still others believe that singularities do not exist, and that their existence in general relativity does not matter, since general relativity is already believed to be an incomplete theory.
According to general relativity, every black hole has a singularity inside. For a non-rotating black hole, this region takes the shape of a single point; for a rotating black hole it is smeared out to form a ring singularity that lies in the plane of rotation. In both cases, the singular region has zero volume. All of the mass of the black hole ends up in the singularity. Since the singularity has nonzero mass in an infinitely small space, it can be thought of as having infinite density.
Chaotic oscillations of spacetime experienced by an object approaching a gravitational singularity
Observers falling into a Schwarzschild black hole (i.e., non-rotating and not charged) cannot avoid being carried into the singularity once they cross the event horizon. As they fall further into the black hole, they will be torn apart by the growing tidal forces in a process sometimes referred to as spaghettification or the noodle effect. Eventually, they will reach the singularity and be crushed into an infinitely small point.
Although in theory, the interior of a Schwarzschild black hole curves inwards towards a sharp point at the singularity, this model is only true when the spacetime inside the black hole had not been perturbed. Any perturbations, such as those caused by matter or radiation falling in, would cause space to oscillate chaotically near the singularity. Any matter falling in would experience intense tidal forces rapidly changing in direction, all while being compressed into an increasingly small volume.
In the case of a charged or rotating black hole, it is possible to avoid the singularity. Extending these solutions as far as possible reveals the hypothetical possibility of exiting the black hole into a different spacetime with the black hole acting as a wormhole. The possibility of travelling to another universe is, however, only theoretical, since any perturbation would destroy this possibility. It also appears to be possible to follow closed timelike curves (returning to one's own past) around the Kerr singularity, which leads to problems with causality like the grandfather paradox. However, processes inside the black hole, such as quantum gravity effects or mass inflation, might prevent closed timelike curves from arising.
To solve technical issues with general relativity, some models of gravity do not include black hole singularities. These theoretical black holes without singularities are called regular, or nonsingular, black holes. For example, the fuzzball model, based on string theory, states that black holes are actually made up of quantum microstates and need not have a singularity or an event horizon. The theory of loop quantum gravity proposes that the curvature and density at the center of a black hole is large, but not infinite.
Types
Gravitational singularity
There are multiple types of singularities, each with different physical features that have characteristics relevant to the theories from which they originally emerged, such as the different shapes of the singularities, conical and curved. They have also been hypothesized to occur without event horizons, structures that delineate one spacetime section from another in which events cannot affect past the horizon; these are called naked.
Conical
A conical singularity occurs when there is a point where the limit of some diffeomorphism invariant quantity does not exist or is infinite, in which case spacetime is not smooth at the point of the limit itself. Thus, spacetime looks like a cone around this point, where the singularity is located at the tip of the cone. The metric can be finite everywhere the coordinate system is used.
An example of such a conical singularity is a cosmic string and the central singularity of a Schwarzschild black hole.
Curvature
A simple illustration of a non-spinning black hole and its singularity
Solutions to the equations of general relativity or another theory of gravity (such as supergravity) often result in encountering points where the metric blows up to infinity. However, many of these points are completely regular, and the infinities are merely a result of using an inappropriate coordinate system at this point. To test whether there is a singularity at a certain point, one must check whether at this point diffeomorphism invariant quantities (i.e. scalars) become infinite. Such quantities are the same in every coordinate system, so these infinities will not "go away" by a change of coordinates.
An example is the Schwarzschild solution that describes a non-rotating, uncharged black hole. In coordinate systems convenient for working in regions far away from the black hole, a part of the metric becomes infinite at the event horizon. However, spacetime at the event horizon is regular. The regularity becomes evident when changing to another coordinate system (such as the Kruskal coordinates), where the metric is perfectly smooth. On the other hand, in the center of the black hole, where the metric becomes infinite as well, the solutions suggest a singularity exists. The existence of the singularity can be verified by noting that the Kretschmann scalar, being the square of the Riemann tensor i.e. ${\displaystyle R{\mu \nu \rho \sigma }R^{\mu \nu \rho \sigma }}$, which is diffeomorphism invariant, is infinite.
While in a non-rotating black hole the singularity occurs at a single point in the model coordinates, called a "point singularity", in a rotating black hole, also known as a Kerr black hole, the singularity occurs on a ring (a circular line), known as a "ring singularity". Such a singularity may also theoretically become a wormhole.
More generally, a spacetime is considered singular if it is geodesically incomplete, meaning that there are freely-falling particles whose motion cannot be determined beyond a finite time, being after the point of reaching the singularity. For example, any observer inside the event horizon of a non-rotating black hole would fall into its center within a finite period of time. The classical version of the Big Bang cosmological model of the universe contains a causal singularity at the start of time (t=0), where all time-like geodesics have no extensions into the past. Extrapolating backward to this hypothetical time 0 results in a universe with all spatial dimensions of size zero, infinite density, infinite temperature, and infinite spacetime curvature.
Naked singularity
Until the early 1990s, it was widely believed that general relativity hides every singularity behind an event horizon, making naked singularities impossible. This is referred to as the cosmic censorship hypothesis. However, in 1991, physicists Stuart Shapiro and Saul Teukolsky performed computer simulations of a rotating plane of dust that indicated that general relativity might allow for "naked" singularities. What these objects would actually look like in such a model is unknown. Nor is it known whether singularities would still arise if the simplifying assumptions used to make the simulation were removed. However, it is hypothesized that light entering a singularity would similarly have its geodesics terminated, thus making the naked singularity look like a black hole.
Disappearing event horizons exist in the Kerr metric, which is a spinning black hole in a vacuum, if the angular momentum (${\displaystyle J}$) is high enough. Transforming the Kerr metric to Boyer–Lindquist coordinates, it can be shown that the coordinate (which is not the radius) of the event horizon is, ${\displaystyle r{\pm }=\mu \pm \left(\mu ^{2}-a^{2}\right)^{1/2}}$, where ${\displaystyle \mu =GM/c^{2}}$, and ${\displaystyle a=J/Mc}$. In this case, "event horizons disappear" means when the solutions are complex for ${\displaystyle r{\pm }}$, or ${\displaystyle \mu ^{2}<a^{2}}$. However, this corresponds to a case where ${\displaystyle J}$ exceeds ${\displaystyle GM^{2}/c}$ (or in Planck units, ${\displaystyle J>M^{2}}$); i.e. the spin exceeds what is normally viewed as the upper limit of its physically possible values.
Similarly, disappearing event horizons can also be seen with the Reissner–Nordström geometry of a charged black hole if the charge (${\displaystyle Q}$) is high enough. In this metric, it can be shown that the singularities occur at ${\displaystyle r{\pm }=\mu \pm \left(\mu ^{2}-q^{2}\right)^{1/2}}$, where ${\displaystyle \mu =GM/c^{2}}$, and ${\displaystyle q^{2}=GQ^{2}/\left(4\pi \epsilon {0}c^{4}\right)}$. Of the three possible cases for the relative values of ${\displaystyle \mu }$ and ${\displaystyle q}$, the case where ${\displaystyle \mu ^{2}<q^{2}}$ causes both ${\displaystyle r{\pm }}$ to be complex. This means the metric is regular for all positive values of ${\displaystyle r}$, or in other words, the singularity has no event horizon. However, this corresponds to a case where ${\displaystyle Q/{\sqrt {4\pi \epsilon {0}}}}$ exceeds ${\displaystyle M{\sqrt {G}}}$ (or in Planck units, ${\displaystyle Q>M}$); i.e. the charge exceeds what is normally viewed as the upper limit of its physically possible values. Also, actual astrophysical black holes are not expected to possess any appreciable charge.
A black hole possessing the lowest ${\displaystyle M}$ value consistent with its ${\displaystyle J}$ and ${\displaystyle Q}$ values and the limits noted above; i.e., one just at the point of losing its event horizon, is termed extremal.