Schwarzschild radius
Template:Short description Template:Use dmy dates
The Schwarzschild radius is a parameter in the Schwarzschild solution to Einstein's field equations that corresponds to the radius of a sphere in flat space that has the same surface area as that of the event horizon of a Schwarzschild black hole of a given mass. It is a characteristic quantity that may be associated with any quantity of mass. The Schwarzschild radius was named after the German astronomer Karl Schwarzschild, who calculated this solution for the theory of general relativity in 1916.
The Schwarzschild radius is given as <math display="block"> r_\text{s} = \frac{2 G M}{c^2} ,</math> where G is the Newtonian constant of gravitation, M is the mass of the object, and c is the speed of light.<ref>Template:Cite book</ref><ref>Template:Cite book</ref>
HistoryEdit
In 1916, Karl Schwarzschild obtained an exact solution<ref>Template:Cite journal</ref><ref>Template:Cite journal</ref> to the Einstein field equations for the gravitational field outside a non-rotating, spherically symmetric body with mass <math>M</math> (see Schwarzschild metric). The solution contained terms of the form Template:Tmath and Template:Tmath, which have singularities at <math>r = 0</math> and <math> r=r_\text{s}</math> respectively. The <math>r_\text{s}</math> has come to be known as the Schwarzschild radius. The physical significance of these singularities was debated for decades. It was found that the one at <math> r = r_\text{s}</math> is a coordinate singularity, meaning that it is an artifact of the particular system of coordinates that was used; while the one at <math>r=0</math> is a spacetime singularity and cannot be removed.<ref>Template:Cite book</ref> The Schwarzschild radius is nonetheless a physically relevant quantity, as noted above and below.
This expression had previously been calculated, using Newtonian mechanics, as the radius of a spherically symmetric body at which the escape velocity was equal to the speed of light. It had been identified in the 18th century by John Michell<ref name="Schaffer">Template:Cite journal</ref> and Pierre-Simon Laplace.<ref>Template:Cite journal</ref>
ParametersEdit
The Schwarzschild radius of an object is proportional to its mass. Accordingly, the Sun has a Schwarzschild radius of approximately Template:Convert,<ref name="Anderson">Template:Cite encyclopedia</ref> whereas Earth's is approximately Template:Convert<ref name="Anderson" /> and the Moon's is approximately Template:Convert.
DerivationEdit
{{#invoke:Labelled list hatnote|labelledList|Main article|Main articles|Main page|Main pages}}
Black hole classification by Schwarzschild radiusEdit
| Class | Approx. mass |
Approx. radius |
|---|---|---|
| Supermassive black hole | 105–1011 MSun | 0.002–2000 AU |
| Intermediate-mass black hole | Template:Val | Template:Val ≈ RMars |
| Stellar black hole | 10 MSun | 30 km |
| Micro black hole | up to MMoon | up to 0.1 mm |
Any object whose radius is smaller than its Schwarzschild radius is called a black hole.<ref>Template:Cite book</ref>Template:Rp The surface at the Schwarzschild radius acts as an event horizon in a non-rotating body (a rotating black hole operates slightly differently). Neither light nor particles can escape through this surface from the region inside, hence the name "black hole".
Black holes can be classified based on their Schwarzschild radius, or equivalently, by their density, where density is defined as mass of a black hole divided by the volume of its Schwarzschild sphere. As the Schwarzschild radius is linearly related to mass, while the enclosed volume corresponds to the third power of the radius, small black holes are therefore much more dense than large ones. The volume enclosed in the event horizon of the most massive black holes has an average density lower than main sequence stars.
Supermassive black holeEdit
{{#invoke:Labelled list hatnote|labelledList|Main article|Main articles|Main page|Main pages}} A supermassive black hole (SMBH) is the largest type of black hole, though there are few official criteria on how such an object is considered so, on the order of hundreds of thousands to billions of solar masses. (Supermassive black holes up to 21 billion Template:Solar mass have been detected, such as NGC 4889.)<ref>Template:Cite journal</ref> Unlike stellar mass black holes, supermassive black holes have comparatively low average densities. (Note that a (non-rotating) black hole is a spherical region in space that surrounds the singularity at its center; it is not the singularity itself.) With that in mind, the average density of a supermassive black hole can be less than the density of water.Template:Cn
The Schwarzschild radius of a body is proportional to its mass and therefore to its volume, assuming that the body has a constant mass-density.<ref>Template:Cite book</ref> In contrast, the physical radius of the body is proportional to the cube root of its volume. Therefore, as the body accumulates matter at a given fixed density (in this example, Template:Val, the density of water), its Schwarzschild radius will increase more quickly than its physical radius. When a body of this density has grown to around 136 million solar masses (Template:Solar mass), its physical radius would be overtaken by its Schwarzschild radius, and thus it would form a supermassive black hole.
It is thought that supermassive black holes like these do not form immediately from the singular collapse of a cluster of stars. Instead they may begin life as smaller, stellar-sized black holes and grow larger by the accretion of matter, or even of other black holes.<ref>Template:Cite journal</ref>
The Schwarzschild radius of the supermassive black hole at the Galactic Center of the Milky Way is approximately 12 million kilometres.<ref name="Ghez08"> Template:Cite journal</ref> Its mass is about Template:Solar mass.
Stellar black holeEdit
{{#invoke:Labelled list hatnote|labelledList|Main article|Main articles|Main page|Main pages}} Stellar black holes have much greater average densities than supermassive black holes. If one accumulates matter at nuclear density (the density of the nucleus of an atom, about 1018 kg/m3; neutron stars also reach this density), such an accumulation would fall within its own Schwarzschild radius at about Template:Solar mass and thus would be a stellar black hole.Template:Cn
Micro black holeEdit
{{#invoke:Labelled list hatnote|labelledList|Main article|Main articles|Main page|Main pages}} {{ safesubst:#invoke:Unsubst||date=__DATE__ |$B= Template:Ambox }} A small mass has an extremely small Schwarzschild radius. A black hole of mass similar to that of Mount Everest,<ref name="SST">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> Template:Val, would have a Schwarzschild radius much smaller than a nanometre.Template:Cn The Schwarzschild radius would be 2 × Template:Val × Template:Val / (Template:Val)2 = Template:Val = Template:Val. Its average density at that size would be so high that no known mechanism could form such extremely compact objects. Such black holes might possibly have been formed in an early stage of the evolution of the universe, just after the Big Bang, when densities of matter were extremely high. Therefore, these hypothetical miniature black holes are called primordial black holes.Template:Cn
Other usesEdit
In gravitational time dilationEdit
Gravitational time dilation near a large, slowly rotating, nearly spherical body, such as the Earth or Sun can be reasonably approximated as follows:<ref>Template:Cite book</ref> <math display="block"> \frac{t_r}{t} = \sqrt{1 - \frac{r_\mathrm{s}}{r}} </math> where:
- Template:Var is the elapsed time for an observer at radial coordinate r within the gravitational field;
- Template:Var is the elapsed time for an observer distant from the massive object (and therefore outside of the gravitational field);
- Template:Var is the radial coordinate of the observer (which is analogous to the classical distance from the center of the object);
- Template:Math is the Schwarzschild radius.
Compton wavelength intersectionEdit
The Schwarzschild radius (Template:Tmath) and the Compton wavelength (Template:Tmath) corresponding to a given mass are similar when the mass is around one Planck mass (Template:Tmath), when both are of the same order as the Planck length (<math display="inline">\sqrt{\hbar G/c^3}</math>).
Calculating the maximum volume and radius possible given a density before a black hole formsEdit
The Schwarzschild radius equation can be manipulated to yield an expression that gives the largest possible radius from an input density that doesn't form a black hole. Taking the input density as Template:Math,
- <math>r_\text{s} = \sqrt{\frac{3 c^{2}}{8 \pi G \rho}}.</math>
For example, the density of water is Template:Val. This means the largest amount of water you can have without forming a black hole would have a radius of Template:Val (about 2.67 AU).
See alsoEdit
- Black hole, a general survey
- Chandrasekhar limit, a second requirement for black hole formation
- John Michell
Classification of black holes by type:
- Static or Schwarzschild black hole
- Rotating or Kerr black hole
- Charged black hole or Newman black hole and Kerr–Newman black hole
A classification of black holes by mass:
- Micro black hole and extra-dimensional black hole
- Planck length
- Primordial black hole, a hypothetical leftover of the Big Bang
- Stellar black hole, which could either be a static black hole or a rotating black hole
- Supermassive black hole, which could also either be a static black hole or a rotating black hole
- Visible universe, if its density is the critical density, as a hypothetical black hole
- Virtual black hole