The Schwarzschild radius (sometimes historically referred to as the gravitational radius) is a physical parameter that shows up in the Schwarzschild solution to Einstein's field equations, corresponding to the radius defining the event horizon of a Schwarzschild black hole. It is a characteristic radius associated with every quantity of mass. The Schwarzschild radius (Sch. R) was named after the German astronomer Karl Schwarzschild, who calculated this exact solution for the theory of general relativity in 1916.

The Schwarzschild radius is given as

\( {\displaystyle r_{s}={\frac {2GM}{c^{2}}},} \)

where G is the gravitational constant, M is the object mass, and c is the speed of light.[1]

History

In 1916, Karl Schwarzschild obtained the exact solution[2][3] to Einstein's field equations for the gravitational field outside a non-rotating, spherically symmetric body with mass M (see Schwarzschild metric). The solution contained terms of the form \( {\displaystyle 1-{r_{s}}/r} \) and \( {\displaystyle {\frac {1}{1-{r_{s}}/r}}} \), which become singular at \( {\displaystyle r=0} \) and \( {\displaystyle r=r_{s}} \) respectively. The \( r_{s} \) 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 \( {\displaystyle r=r_{s}} \) is a coordinate singularity, meaning that it is an artefact of the particular system of coordinates that were used, while the one at \( {\displaystyle r=0} \) is physical, and cannot be removed.[4] 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[5] and by 19th century astronomers such as Pierre-Simon Laplace.[6]

Parameters

The Schwarzschild radius of an object is proportional to the mass. Accordingly, the Sun has a Schwarzschild radius of approximately 3.0 km (1.9 mi), whereas Earth's is only about 9 mm (0.35 in) and the Moon's is about 0.1 mm (0.0039 in). The observable universe's mass has a Schwarzschild radius of approximately 13.7 billion light-years.[7][8]

Object Mass: M {\displaystyle M} M Schwarzschild radius: \( {\displaystyle {\frac {2GM}{c^{2}}}} \) Schwarzschild density: \( {\displaystyle {\frac {3c^{6}}{32\pi G^{3}M^{2}}}} \) or \( {\displaystyle {\frac {3c^{2}}{8\pi Gr^{2}}}} \)

Observable universe[7] 8.8×1052 kg 1.3×1026 m (13.7 billion ly) 9.5×10−27 kg/m3

Milky Way 1.6×1042 kg 2.4×1015 m (~0.25 ly) 0.000029 kg/m3

TON 618 (largest known black hole) 1.3×1041 kg 1.9×1014 m (~1300 AU) 0.0045 kg/m3

SMBH in NGC 4889 4.2×1040 kg 6.2×1013 m 0.042 kg/m3

SMBH in Messier 87[9] 1.3×1040 kg 1.9×1013 m 0.44 kg/m3

SMBH in Andromeda Galaxy[10] 3.4×1038 kg 5.0×1011 m 640 kg/m3

Sagittarius A* (SMBH in Milky Way) 8.2×1036 kg 1.2×1010 m 1.1×106 kg/m3

Sun 1.99×1030 kg 2.95×103 m 1.84×1019 kg/m3

Jupiter 1.90×1027 kg 2.82 meters 2.02×1025 kg/m3

Earth 5.97×1024 kg 8.87×10−3 m 2.04×1030 kg/m3

Moon 7.35×1022 kg 1.09×10−4 m 1.35×1034 kg/m3

Human 70 kilograms 1.04×10−25 m 1.49×1076 kg/m3

Big Mac 0.215 kilograms 3.19×10−28 m 1.58×1081 kg/m3

Planck mass 2.18×10−8 kg 3.23×10−35 m 1.54×1095 kg/m3

Derivation

Main article: Deriving the Schwarzschild solution

Black hole classification by Schwarzschild radius

Black hole classifications Class Approx.

mass Approx.

radius

Supermassive black hole 105–1010 MSun 0.001–400 AU

Intermediate-mass black hole 103 MSun 103 km ≈ REarth

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. 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 hole

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 (2.1 × 10^{10}) M☉ have been detected, such as NGC 4889.)[11] 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.

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.[12] 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, 997 kg/m^{3}, 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 (1.36 × 10^{8}) M☉, 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.

The Schwarzschild radius of the supermassive black hole at the Galactic Center is approximately 12 million kilometres.[13]

Stellar black hole

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 10^{18} kg/m3; neutron stars also reach this density), such an accumulation would fall within its own Schwarzschild radius at about 3 M☉ and thus would be a stellar black hole.

Primordial black hole

A small mass has an extremely small Schwarzschild radius. A mass similar to Mount Everest[14][note 1] has a Schwarzschild radius much smaller than a nanometre.[note 2] 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 be formed in an early stage of the evolution of the universe, just after the Big Bang, when densities were extremely high. Therefore, these hypothetical miniature black holes are called primordial black holes.

Other uses

In gravitational time dilation

Gravitational time dilation near a large, slowly rotating, nearly spherical body, such as the Earth or Sun can be reasonably approximated using the Schwarzschild radius as follows:

\( {\frac {t_{r}}{t}}={\sqrt {1-{\frac {r_{\mathrm {s} }}{r}}}} \)

where:

tr is the elapsed time for an observer at radial coordinate r within the gravitational field;

t is the elapsed time for an observer distant from the massive object (and therefore outside of the gravitational field);

r is the radial coordinate of the observer (which is analogous to the classical distance from the center of the object);

rs is the Schwarzschild radius.

The results of the Pound–Rebka experiment in 1959 were found to be consistent with predictions made by general relativity. By measuring Earth's gravitational time dilation, this experiment indirectly measured

Earth's Schwarzschild radius.

In Newtonian gravitational fields

The Newtonian gravitational field near a large, slowly rotating, nearly spherical body can be reasonably approximated using the Schwarzschild radius as follows:

\( {\displaystyle mg={\frac {GMm}{r^{2}}}\quad \Rightarrow \quad gr^{2}=GM} \)

and

\( {\displaystyle r_{\mathrm {s} }={\frac {2GM}{c^{2}}}\quad \Rightarrow \quad r_{\mathrm {s} }c^{2}=2GM} \)

Therefore, on dividing above by below:

\( {\frac {g}{r_{\mathrm {s} }}}\left({\frac {r}{c}}\right)^{2}={\frac {1}{2}} \)

where:

g is the gravitational acceleration at radial coordinate r;

rs is the Schwarzschild radius of the gravitating central body;

r is the radial coordinate;

c is the speed of light in vacuum.

On the surface of the Earth:

\( {\frac {9.80665\ \mathrm {m} /\mathrm {s} ^{2}}{8.870056\ \mathrm {mm} }}\left({\frac {6375416\ \mathrm {m} }{299792458\ \mathrm {m} /\mathrm {s} }}\right)^{2}=\left(1105.59\ \mathrm {s} ^{-2}\right)\left(0.0212661\ \mathrm {s} \right)^{2}={\frac {1}{2}}. \)

In Keplerian orbits

For all circular orbits around a given central body:

\( {\displaystyle {\frac {mv^{2}}{r}}={\text{Centripetal force}}={\text{Gravitational force}}={\frac {GMm}{r^{2}}}} \)

Therefore,

\( {\displaystyle rv^{2}=GM,} \)

but

\( {\displaystyle r_{\mathrm {s} }c^{2}=2GM} \) (derived above)

Therefore,

\( {\frac {r}{r_{\mathrm {s} }}}\left({\frac {v}{c}}\right)^{2}={\frac {1}{2}} \)

where:

r is the orbit radius;

rs is the Schwarzschild radius of the gravitating central body;

v is the orbital speed;

c is the speed of light in vacuum.

This equality can be generalized to elliptic orbits as follows:

\( {\frac {a}{r_{\mathrm {s} }}}\left({\frac {2\pi a}{cT}}\right)^{2}={\frac {1}{2}} \)

where:

a is the semi-major axis;

T is the orbital period.

For the Earth, as a planet orbiting the Sun:

\( {\displaystyle {\frac {1\,\mathrm {AU} }{2953.25\,\mathrm {m} }}\left({\frac {2\pi \,\mathrm {AU} }{\mathrm {light\,year} }}\right)^{2}=\left(50655379.7\right)\left(9.8714403\times 10^{-9}\right)={\frac {1}{2}}.} \)

Relativistic circular orbits and the photon sphere

The Keplerian equation for circular orbits can be generalized to the relativistic equation for circular orbits by accounting for time dilation in the velocity term:

\( {\frac {r}{r_{s}}}\left({\frac {v}{c}}{\sqrt {1-{\frac {r_{s}}{r}}}}\right)^{2}={\frac {1}{2}} \)

\( {\frac {r}{r_{s}}}\left({\frac {v}{c}}\right)^{2}\left(1-{\frac {r_{s}}{r}}\right)={\frac {1}{2}} \)

\( \left({\frac {v}{c}}\right)^{2}\left({\frac {r}{r_{s}}}-1\right)={\frac {1}{2}}. \)

This final equation indicates that an object orbiting at the speed of light would have an orbital radius of 1.5 times the Schwarzschild radius. This is a special orbit known as the photon sphere.

Schwarzschild radius for Planck mass

For the Planck mass \( {\displaystyle m_{\rm {P}}={\sqrt {\hbar c/G}}} \) , the Schwarzschild radius \( {\displaystyle r_{\rm {S}}=2\ell _{\rm {P}}} \) and the Compton wavelength \( {\displaystyle \lambda _{\rm {C}}=2\pi \ell _{\rm {P}}} \) are of the same order as the Planck length \( {\displaystyle \ell _{\rm {P}}={\sqrt {\hbar G/c^{3}}}}. \)

Schwarzschild radius and the uncertainty principle on the Planck scale [15]

\( {\displaystyle r_{s}={\frac {2GM}{c^{2}}}={\frac {2G}{c^{3}}}Mc={\frac {2G}{c^{3}}}P_{0}\approx {\frac {2G}{c^{3}}}{\frac {\hbar }{2r}}={\frac {\ell _{P}^{2}}{r}}.} \)

Therefore, \( {\displaystyle r_{s}r\sim \ell _{P}^{2}} \) or \( {\displaystyle \Delta r_{s}\Delta r\geq \ell _{P}^{2}} \)

See also

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

Notes

Using these values,[14] one can calculate a mass estimate of 6.3715e14 kg.

One can calculate the Schwarzschild radius: 2 × 6.6738e-11 m3 kg−1 s−2 × 6.3715e14 kg / (299 792 458 m s−1)2 = 9.46e-13 m, or 9.46e-4 nm.

References

Kutner, Marc (2003). Astronomy: A Physical Perspective. Cambridge University Press. p. 148. ISBN 9780521529273.

K. Schwarzschild, "Über das Gravitationsfeld eines Massenpunktes nach der Einsteinschen Theorie", Sitzungsberichte der Deutschen Akademie der Wissenschaften zu Berlin, Klasse fur Mathematik, Physik, und Technik (1916) pp 189.

K. Schwarzschild, "Über das Gravitationsfeld einer Kugel aus inkompressibler Flussigkeit nach der Einsteinschen Theorie", Sitzungsberichte der Deutschen Akademie der Wissenschaften zu Berlin, Klasse fur Mathematik, Physik, und Technik (1916) pp 424.

Wald, Robert (1984). General Relativity. The University of Chicago Press. pp. 152–153. ISBN 978-0-226-87033-5.

Schaffer, Simon (1979). "John Michell and Black Holes". Journal for the History of Astronomy. 10: 42–43. Bibcode:1979JHA....10...42S. doi:10.1177/002182867901000104. S2CID 123958527. Retrieved 4 June 2018.

Colin Montgomery, Wayne Orchiston and Ian Whittingham, "Michell, Laplace and the origin of the Black Hole Concept", Journal of Astronomical History and Heritage, 12(2), 90–96 (2009).

Valev, Dimitar (October 2008). "Consequences from conservation of the total density of the universe during the expansion".arXiv:1008.0933 [physics.gen-ph].

Deza, Michel Marie; Deza, Elena (Oct 28, 2012). Encyclopedia of Distances (2nd ed.). Heidelberg: Springer Science & Business Media. p. 452. doi:10.1007/978-3-642-30958-8. ISBN 978-3-642-30958-8. Retrieved 8 December 2014.

Event Horizon Telescope Collaboration (2019). "First M87 Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole". Astrophysical Journal Letters. 875 (1): L1.arXiv:1906.11238. Bibcode:2019ApJ...875L...1E. doi:10.3847/2041-8213/AB0EC7. 6.5(7) × 109 M☉ = 1.29(14)×1040 kg.

Bender, Ralf; Kormendy, John; Bower, Gary; et al. (2005). "HST STIS Spectroscopy of the Triple Nucleus of M31: Two Nested Disks in Keplerian Rotation around a Supermassive Black Hole". Astrophysical Journal. 631 (1): 280–300.arXiv:astro-ph/0509839. Bibcode:2005ApJ...631..280B. doi:10.1086/432434. S2CID 53415285. 1.7(6) × 108 M☉ = 0.34(12)×1039 kg.

McConnell, Nicholas J. (2011-12-08). "Two ten-billion-solar-mass black holes at the centres of giant elliptical galaxies". Nature. 480 (7376): 215–218.arXiv:1112.1078. Bibcode:2011Natur.480..215M. doi:10.1038/nature10636. PMID 22158244. S2CID 4408896.

Robert H. Sanders (2013). Revealing the Heart of the Galaxy: The Milky Way and its Black Hole. Cambridge University Press. p. 36. ISBN 978-1-107-51274-0.

Ghez, A. M.; et al. (December 2008). "Measuring Distance and Properties of the Milky Way's Central Supermassive Black Hole with Stellar Orbits". Astrophysical Journal. 689 (2): 1044–1062.arXiv:0808.2870. Bibcode:2008ApJ...689.1044G. doi:10.1086/592738. S2CID 18335611.

"How does the mass of one mole of M&M's compare to the mass of Mount Everest?" (PDF). School of Science and Technology, Singapore. March 2003. Archived from the original (PDF) on 10 December 2014. Retrieved 8 December 2014. "If Mount Everest is assumed* to be a cone of height 8850 m and radius 5000 m, then its volume can be calculated using the following equation:

volume = πr2h/3 [...] Mount Everest is composed of granite, which has a density of 2750 kg m−3."

Klimets AP, Philosophy Documentation Center, Western University-Canada, 2017, pp.25-30

vte

Black holes

Types

Schwarzschild Rotating Charged Virtual Kugelblitz Primordial Planck particle

Size

Micro

Extremal Electron Stellar

Microquasar Intermediate-mass Supermassive

Active galactic nucleus Quasar Blazar

Formation

Stellar evolution Gravitational collapse Neutron star

Related links Tolman–Oppenheimer–Volkoff limit White dwarf

Related links Supernova

Related links Hypernova Gamma-ray burst Binary black hole

Properties

Gravitational singularity

Ring singularity Theorems Event horizon Photon sphere Innermost stable circular orbit Ergosphere

Penrose process Blandford–Znajek process Accretion disk Hawking radiation Gravitational lens Bondi accretion M–sigma relation Quasi-periodic oscillation Thermodynamics

Immirzi parameter Schwarzschild radius Spaghettification

Issues

Black hole complementarity Information paradox Cosmic censorship ER=EPR Final parsec problem Firewall (physics) Holographic principle No-hair theorem

Metrics

Schwarzschild (Derivation) Kerr Reissner–Nordström Kerr–Newman Hayward

Alternatives

Nonsingular black hole models Black star Dark star Dark-energy star Gravastar Magnetospheric eternally collapsing object Planck star Q star Fuzzball

Analogs

Optical black hole Sonic black hole

Lists

Black holes Most massive Nearest Quasars Microquasars

Related

Black Hole Initiative Black hole starship Compact star Exotic star

Quark star Preon star Gamma-ray burst progenitors Gravity well Hypercompact stellar system Membrane paradigm Naked singularity Quasi-star Rossi X-ray Timing Explorer Timeline of black hole physics White hole Wormhole

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