Schwarzschild Radius Calculator

Calculation Mode

Quick Presets — click to fill:

Mass (M)

Enter the mass of the object. Default unit is solar masses (M☉).

Actual Physical Radius (optional — for Black Hole Check)

Enter the object's actual radius (in km) to check whether it qualifies as a black hole.

Formula: r_s = 2GM / c²

r_s = 2GM / c²

G = 6.674 × 10⁻¹¹ N·m²/kg²

c = 2.998 × 10⁸ m/s

Enter a Mass to Begin

Select a preset object (Earth, Sun, Sagittarius A*) or enter any mass value. The calculator will instantly show the Schwarzschild radius, surface gravity, density, photon sphere, ISCO, and more.

Last updated October 20, 2018

Compute the event horizon radius for any mass — from atoms to supermassive black holes

The Schwarzschild radius is one of the most profound concepts in modern astrophysics. It defines the critical boundary — called the event horizon — at which the escape velocity from an object's gravitational field equals the speed of light. Any object compressed to within its Schwarzschild radius becomes a black hole, a region of spacetime from which nothing, not even light, can escape. Understanding this radius is fundamental to studying black holes, neutron stars, and the extreme limits of gravitational physics. Karl Schwarzschild derived this solution in 1916, just weeks after Einstein published his general theory of relativity, while Schwarzschild was serving on the Russian front during World War I. His solution described the spacetime geometry outside a perfectly spherical, non-rotating mass. The resulting radius bears his name and remains one of the most elegant results in theoretical physics. It tells us that for any mass — a pebble, a planet, a star — there exists a corresponding Schwarzschild radius, though compressing macroscopic objects to that scale requires conditions found only in nature's most extreme environments. For everyday objects, the Schwarzschild radius is extraordinarily small. The entire Earth compressed to a marble-sized sphere of about 8.87 millimeters would become a black hole. The Sun would need to be squeezed into a ball roughly 2.95 kilometers across — smaller than many cities. Meanwhile, supermassive black holes like Sagittarius A* at the center of our Milky Way galaxy, with a mass of about 4.15 million solar masses, have a Schwarzschild radius of approximately 12.27 million kilometers — larger than the Sun itself. This calculator uses the exact formula rs = 2GM/c², where G is Newton's gravitational constant (6.674 × 10⁻¹¹ N·m²/kg²), M is the mass of the object in kilograms, and c is the speed of light (2.998 × 10⁸ m/s). You can input mass in solar masses, Earth masses, Jupiter masses, or kilograms, and the results include not just the Schwarzschild radius but also several derived quantities: the surface gravity at the event horizon, the average density of the hypothetical black hole, the Hawking radiation temperature, the photon sphere radius, and the innermost stable circular orbit (ISCO) distance. The surface gravity at the event horizon is given by g = c⁴ / (4GM). Counterintuitively, this gravity decreases for more massive black holes. A stellar black hole of 10 solar masses has enormous surface gravity at its event horizon, while a supermassive black hole like M87* has surface gravity comparable to or less than Earth's gravity at the event horizon — though tidal forces are still lethal well beyond the horizon for stellar-mass black holes. The average density of a black hole — computed as the mass divided by the volume of a sphere with radius rs — reveals another surprising fact: as black holes grow more massive, they become less dense on average. A one-solar-mass black hole would have an average density of about 1.85 × 10¹⁹ kg/m³, far denser than nuclear matter. But a billion-solar-mass supermassive black hole would have an average density less than that of water. The largest black holes are, on average, surprisingly diffuse objects. Hawking radiation, predicted by Stephen Hawking in 1974, is a quantum mechanical effect by which black holes slowly emit thermal radiation and lose mass over astronomical timescales. The temperature of this radiation is T_H = ℏc³ / (8πGMk_B). For stellar-mass black holes, this temperature is a tiny fraction of a kelvin — essentially indistinguishable from absolute zero and undetectable against the cosmic microwave background. Only primordial black holes of subatomic mass would be radiating detectably today. The photon sphere, at a radius of 1.5 × rs, is where photons can orbit the black hole in unstable circular orbits — photons nudged inward spiral into the black hole while those nudged outward escape to infinity. The ISCO (Innermost Stable Circular Orbit) at 3 × rs is the closest stable circular orbit for matter around a non-rotating black hole; within this radius, any in-falling matter spirals rapidly into the event horizon.

Understanding the Schwarzschild Radius

What Is the Schwarzschild Radius?

The Schwarzschild radius (symbol: rs) is the radius of the event horizon — the point of no return around a black hole. It represents the critical size to which any mass M must be compressed to become a black hole. Once compressed beyond this radius, the escape velocity at the surface exceeds the speed of light, meaning nothing can escape. Named after physicist Karl Schwarzschild who derived it in 1916, rs = 2GM/c² applies to any non-rotating, uncharged, spherically symmetric mass. The concept is purely gravitational: every object in the universe has a corresponding Schwarzschild radius, but for most objects that radius is far smaller than atomic scales, making their compression into a black hole physically impossible under known conditions.

How Is It Calculated?

The primary formula is rs = 2GM/c², derived from Einstein's general theory of relativity. G = 6.674 × 10⁻¹¹ N·m²/kg² is Newton's gravitational constant, M is the object's mass in kilograms, and c = 2.998 × 10⁸ m/s is the speed of light. For solar masses, this simplifies to rs ≈ 2,953 meters per solar mass. Surface gravity at the event horizon is g = c⁴ / (4GM). Average density is ρ = 3c⁶ / (32πG³M²), which shows that density decreases with increasing mass. Hawking temperature is T_H = ℏc³ / (8πGMk_B). The photon sphere is at 1.5 × rs and the ISCO is at 3 × rs. All computations use standard SI units before converting to human-friendly units.

Why Does It Matter?

The Schwarzschild radius is the cornerstone of black hole physics. It defines where extreme curvature of spacetime creates an inescapable region. In stellar evolution, it determines whether a collapsed stellar remnant becomes a neutron star (if its radius stays above rs) or a black hole (if compression continues past rs). It enables astronomers to calculate the expected event horizon size from measured black hole masses — validated spectacularly by the Event Horizon Telescope's images of M87* and Sagittarius A*. In gravitational wave astronomy, knowledge of rs helps interpret inspiral and merger events. In technology, GPS satellites require relativistic corrections that originate from the same general relativistic framework that gives us the Schwarzschild radius.

Limitations and Caveats

The Schwarzschild radius formula applies strictly to non-rotating, uncharged black holes in vacuum. Real astrophysical black holes rotate (Kerr metric) and may carry charge (Kerr-Newman metric). A rotating black hole's event horizon is smaller than its Schwarzschild radius and depends on the spin parameter. For rapidly rotating black holes like those powering quasars, the ISCO shrinks to as close as rs/2. Additionally, quantum effects (Hawking radiation) become significant only for extremely small black holes — stellar and larger black holes evaporate on timescales far exceeding the age of the universe. The formula also assumes spacetime outside a perfect sphere; real objects have irregular mass distributions. Finally, no known physical process can compress macroscopic objects like planets or stars below their Schwarzschild radius from the outside — black holes form through gravitational collapse of massive stars.

Key Schwarzschild Radius Formulas

Schwarzschild Radius

Rs = 2GM / c²

The event horizon radius for a non-rotating, uncharged black hole. G is Newton's gravitational constant (6.674 × 10⁻¹¹ N·m²/kg²), M is mass, and c is the speed of light (2.998 × 10⁸ m/s).

Event Horizon Surface Area

A = 4πRs² = 16πG²M² / c⁴

The area of the event horizon sphere. Related to Bekenstein-Hawking entropy, which states that a black hole's entropy is proportional to its event horizon area.

Hawking Temperature

T_H = ℏc³ / (8πGMk_B)

The thermal temperature of Hawking radiation emitted by a black hole. ℏ is the reduced Planck constant, k_B is Boltzmann's constant. Temperature is inversely proportional to mass — smaller black holes are hotter.

Average Density

ρ = 3c⁶ / (32πG³M²)

The average density of a black hole computed as mass divided by the volume of a sphere with radius Rs. Counterintuitively, density decreases with increasing mass.

Black Hole Reference Data

Schwarzschild Radius for Various Masses

Event horizon radius, average density, and Hawking temperature for objects ranging from planetary to supermassive scales.

Object	Mass	Schwarzschild Radius	Average Density (kg/m³)	Hawking Temp (K)
Moon	7.34 × 10²² kg	0.11 mm	1.44 × 10³⁰	1.67 × 10⁻⁷
Earth	5.97 × 10²⁴ kg	8.87 mm	2.04 × 10²⁷	2.05 × 10⁻⁹
Jupiter	1.90 × 10²⁷ kg	2.82 m	2.02 × 10²¹	6.45 × 10⁻¹²
Sun	1.99 × 10³⁰ kg	2.95 km	1.85 × 10¹⁹	6.17 × 10⁻⁸
10 M☉ Stellar BH	1.99 × 10³¹ kg	29.5 km	1.85 × 10¹⁷	6.17 × 10⁻⁹
Sgr A* (4.15M M☉)	8.26 × 10³⁶ kg	12.27 M km	10.7	1.49 × 10⁻¹⁴
M87* (6.5B M☉)	1.29 × 10⁴⁰ kg	19.2 B km	4.38 × 10⁻⁶	9.49 × 10⁻¹⁸

Key Black Hole Orbital Radii

Important orbital radii around a non-rotating (Schwarzschild) black hole, expressed as multiples of Rs.

Feature	Radius	Significance
Event Horizon	1.0 × Rs	Point of no return — escape velocity equals c
Photon Sphere	1.5 × Rs	Unstable circular photon orbits; creates the black hole 'shadow'
ISCO	3.0 × Rs	Innermost stable circular orbit; inner edge of accretion disk
Tidal Disruption (stellar BH)	~10–100 × Rs	Region where tidal forces spaghettify infalling matter
Gravitational Influence	~10⁵–10⁶ × Rs	Sphere of gravitational dominance over surrounding stars

Worked Examples

Schwarzschild Radius of a 10 Solar Mass Black Hole

A stellar black hole formed from a massive star has a remnant mass of 10 solar masses (M = 10 × 1.989 × 10³⁰ kg = 1.989 × 10³¹ kg).

Apply the formula: Rs = 2GM/c² = 2 × 6.674×10⁻¹¹ × 1.989×10³¹ / (2.998×10⁸)²

Numerator: 2 × 6.674×10⁻¹¹ × 1.989×10³¹ = 2.654 × 10²¹

Denominator: (2.998×10⁸)² = 8.988 × 10¹⁶

Rs = 2.654×10²¹ / 8.988×10¹⁶ = 29,530 m ≈ 29.5 km

A 10 solar mass black hole has an event horizon radius of approximately 29.5 km — roughly the size of a small city. Its photon sphere is at 44.3 km and ISCO at 88.6 km.

Earth Compressed to a Black Hole

Earth has a mass of 5.972 × 10²⁴ kg and an actual radius of 6,371 km. What is its Schwarzschild radius?

Rs = 2 × 6.674×10⁻¹¹ × 5.972×10²⁴ / (2.998×10⁸)²

Rs = 7.972×10¹⁴ / 8.988×10¹⁶ = 8.87 × 10⁻³ m = 8.87 mm

Compression ratio: 6,371,000 m / 0.00887 m = 7.18 × 10⁸

Average density at Rs: ρ = M / (4/3 × π × Rs³) = 2.04 × 10²⁷ kg/m³ — denser than nuclear matter

Earth would need to be compressed into a marble just 8.87 mm in radius — 719 million times smaller than its actual size — to become a black hole with a density 2 trillion times that of nuclear matter.

How to Use the Schwarzschild Radius Calculator

Select Calculation Mode

Choose 'Mass to Radius' to compute the Schwarzschild radius from a known mass, or 'Radius to Mass' to find the mass corresponding to a given event horizon radius. Most users will start with Mass to Radius mode.

Enter a Mass or Use a Preset

Type any mass value and select your unit (kg, solar masses, Earth masses, Jupiter masses, or moon masses). Or click one of the quick preset buttons — Moon, Earth, Sun, Stellar BH, Sagittarius A*, M87*, Neutron Star, or Jupiter — to instantly load a real-world example.

Review All Output Values

The results show the Schwarzschild radius in the most readable unit, along with surface gravity at the event horizon, average density, Hawking temperature, photon sphere radius, and ISCO radius. Toggle 'Show Advanced Outputs' for Hawking temperature and orbital radii.

Check Black Hole Status (Optional)

To determine if an object is currently a black hole, enter its actual physical radius in the optional field. The calculator will compare it to the Schwarzschild radius and tell you whether the object is already a black hole or how much it would need to be compressed.

Frequently Asked Questions

What is the Schwarzschild radius of the Sun?

The Sun's Schwarzschild radius is approximately 2.953 kilometers — about the size of a small city. This means if you could compress the entire mass of the Sun (1.989 × 10³⁰ kg) into a sphere just under 3 kilometers in radius, it would become a black hole. In reality, the Sun is far too small and cool to collapse this way; it will eventually become a white dwarf. However, stars with masses above roughly 20-25 solar masses can undergo core collapse and form stellar black holes after supernova explosions.

What is the Schwarzschild radius of Earth?

Earth's Schwarzschild radius is approximately 8.87 millimeters — about the size of a marble or a small grape. The entire mass of Earth (5.972 × 10²⁴ kg) would need to be compressed into a sphere smaller than a centimeter to become a black hole. Earth is nowhere near dense enough to collapse gravitationally; its actual radius of 6,371 kilometers is about 719 million times larger than its Schwarzschild radius. Compressing Earth to a black hole would require energy vastly beyond any naturally occurring process on Earth.

Do supermassive black holes have lower density than water?

Yes — this is one of the most counterintuitive facts in black hole physics. The average density of a black hole is calculated as mass divided by the volume of a sphere with the Schwarzschild radius. Because the Schwarzschild radius scales linearly with mass but volume scales as radius cubed, average density decreases as mass squared. A black hole of about 10 million solar masses has an average density roughly equal to that of water (1,000 kg/m³). Sagittarius A* at 4.15 million solar masses is slightly denser than water on average, while M87* at 6.5 billion solar masses has an average density hundreds of thousands of times lower than air.

What is the photon sphere and why does it matter?

The photon sphere is a spherical region at a radius of 1.5 times the Schwarzschild radius where photons can travel in unstable circular orbits. If a photon is placed at exactly this radius with the right direction, it will orbit indefinitely — but any perturbation causes it to either spiral inward to the event horizon or escape to infinity. The photon sphere is what gives black holes their distinctive 'shadow' seen in Event Horizon Telescope images of M87* and Sagittarius A*. The bright ring of light surrounding the dark shadow corresponds to photons that have orbited the black hole multiple times before escaping toward the observer.

What is Hawking radiation and is it detectable?

Hawking radiation is a theoretical quantum mechanical process by which black holes slowly emit thermal radiation due to quantum effects near the event horizon. Stephen Hawking predicted this in 1974. The temperature of this radiation is inversely proportional to the mass: T_H = ℏc³ / (8πGMk_B). For stellar-mass black holes (~3-10 solar masses), this temperature is roughly 6 × 10⁻⁸ to 2 × 10⁻⁸ kelvin — far colder than the cosmic microwave background at 2.725 K. This means stellar and supermassive black holes are currently absorbing CMB radiation faster than they emit Hawking radiation. Detection is currently impossible; only primordial black holes of asteroid mass or less could be warm enough to detect.

What is the ISCO and why is it important in astrophysics?

The Innermost Stable Circular Orbit (ISCO) is the smallest circular orbit in which a test particle can stably orbit a black hole without spiraling in. For a non-rotating Schwarzschild black hole, the ISCO occurs at 3 times the Schwarzschild radius, or 6GM/c². Inside the ISCO, there are no stable circular orbits; matter falling within this radius spirals rapidly inward. The ISCO is critical in accretion disk physics — the inner edge of the accretion disk that makes black holes shine in X-rays corresponds approximately to the ISCO. For rotating (Kerr) black holes, the ISCO shrinks toward the event horizon as spin increases, which affects how efficiently accreting matter radiates energy before plunging in.

Schwarzschild Radius Calculator