Module 04 • Astrophysical Calculators•General Relativity & Black Holes•

Einstein 1915 • Schwarzschild 1916 • Hawking 1974

Schwarze-Loch-Physik

Explore the extreme astrophysics of black holes through Karl Schwarzschild's exact solution to Einstein's field equations. Calculate the Schwarzschild radius (event horizon) for any celestial mass and discover how intense gravitational curvature warps time near the abyss.

Control Deck & Telemetry

Interactive Relativistic Parameters

Input Fields

Mass (M)1.989e+30 kg

Celestial Presets:

Distance from Black Hole (r) (r)2.00 × Rs

Orbital Distance Presets:

Kerr Spin Parameter (a*)a* = 0.00

0.00 (Static)0.500.99 (Max Kerr)

Ergosphere (Equator):2.95413 km

Outer Horizon (r+):2.95413 km (0.0% reduced)

Ergosphere Depth (Frame-Dragging):0 km

Initializing 3D Spacetime Canvas...

Current Scale Ratio (r / Rs):2.000×•Event Horizon:2.95413 km•Ergosphere:2.95413 km•a* = 0.00

Results

6 Relativistic Physics, Quantum Mechanics & Gravitational Lensing Calculators

Schwarzschild-Radius (Rs = 2GM/c²)Calc 1

Determine the event horizon boundary for any stellar or hypothetical mass

Rs = 2GM / c²

Calculated Schwarzschild Radius (Rs)2GM/c²

2.95413km

In Meters:2,954.127 m

If compressed into a black hole, the Sun would have a radius of ~2.95 km.

Gravitative ZeitdilatationCalc 2

Quantify the slowing of time experienced near a curved gravitational well

t = t₀ / √(1 - Rs/r)

Relativistic Time Dilationt₀ = 1.00 hr

1.4142hours on Earth

Duration:1h 24m 51s

Dilation Factor (γ):1.4142×

Hawking-TemperaturCalc 3

Thermal radiation emitted by quantum effects near the event horizon

T = (1.227 × 10²³) / M

Hawking TemperatureKelvin (K)

6.1689 × 10^-8 K

Nearly absolute zero. Emits virtually imperceptible quantum radiation into the vacuum.

VerdampfungszeitCalc 4

Time required for a black hole to completely radiate away its mass into quantum particles

t_evap ∝ M³

Evaporation LifespanLifespan in Years

2.0974 × 10^67 yrs

Vastly exceeds the current age of the Universe (~13.8 billion years).

Why Smaller Black Holes Evaporate Faster

Smaller black holes evaporate dramatically faster. Because evaporation time scales with M³, as a black hole loses mass it gets hotter and radiates faster, ending in a runaway explosive detonation.

Gezeitenkraft & SpaghettifizierungCalc 5

Differential gravity between head and feet causing extreme vertical stretching

Δg ≈ 2GMh / r³

Observer Height (meters)2 meters (standard human height)

meters (m)

Radial Distance (r):r = 5.908 km

Differential Tidal ForceNewtons (N)

1.8016 × 10^11 N

Gravitational Gradient (Δg):2.5737 × 10^9 m/s²

Fatal Spaghettification: Tidal forces exceed human tensile strength, stretching body into a stream of particles.

Gravitationslinseneffektθ = 4GM / (c²b)

Calculate relativistic light deflection around a curved spacetime gravitational well

θ = 2Rs / b

Deflection Angle (θ)b / Rs = 5.00×

22.919°Degrees

Degrees: 22.9193°

Arcminutes: 1375.16′

Radians: 4.000e-1

Impact Parameter (b)5.00 × Rs

Distance Presets:

Section 02 • Celestial Mechanics•T² = a³ • v_e = √(2GM/r)

Cosmic Mathematics

The universe is built on mathematical equations. Explore the fundamental relationships governing orbital motion, planetary trajectories, and gravitational escape thresholds.

Kepler's Third Law (Orbital Math)T² = a³

Calculate orbital period or distance from the Sun using Johannes Kepler's Harmonic Law

T = √(a³) • a = ∛(T²)

Kepler's Harmonic LawT² = a³

T²(1.000)

a³(1.000)

Harmonic Balance Verified

Semi-Major Axis (a)AU

Distance in Kilometers:1.4960 × 10^8 km

Orbital Period (T)Earth Years

yrs

Equivalent Period:365.25 days

Bidirectional: change distance to calculate period, or change period to calculate distance.

Planetary Presets:

Fluchtgeschwindigkeit (v_e = √(2GM/r))v_e = √(2GM/r)

Determine the minimum speed required to escape the gravitational pull of a celestial body

v_e = √(2 · G · M / r)

Calculated Escape Velocity (v_e)1.00× Earth escape speed

11.19km/s/11,185.978 m/s

Speed in km/h: 40,269.52 km/h

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Acoustic Mach: Mach 32.6

Why the Moon Can't Hold an Atmosphere

The Moon's escape velocity is only ~2.38 km/s (compared to Earth's 11.19 km/s). Under direct sunlight, lunar surface temperatures reach 120°C (393 K), accelerating common atmospheric gas molecules (such as water vapor, nitrogen, oxygen, and carbon dioxide) past their thermal escape thresholds. Without a global magnetic field or sufficient gravitational acceleration, any outgassed atmosphere boils off into interplanetary space over cosmic timescales.

Celestial Presets:

Body Mass (M)5.972e+24 kg

Mean Radius (r)1.00 R⊕

Theoretical Foundations & Astrophysical Insights

Karl Schwarzschild's 1916 Solution

Serving on the Russian front during World War I, German physicist Karl Schwarzschild produced the very first exact analytical solution to Albert Einstein's field equations, discovering the geometry of curved spacetime outside a spherical mass.

Gravitational Redshift & The Event Horizon

As electromagnetic radiation climbs outward from a deep gravitational well, it loses energy and shifts to longer wavelengths. At r = Rs, the redshift becomes infinite: to an outside observer, an infalling object appears to freeze and fade away.

Empirical Astronomical Verification

Once debated as mathematical curiosities, black holes have been verified empirically through stellar kinematics, LIGO gravitational wave detections, and direct shadow imaging of M87* (2019) and Sgr A* (2022) by the Event Horizon Telescope.