⊕ ASTEROID IMPACT SIMULATOR
ADVANCED PHYSICS ENGINE · REAL PLANETARY DATA · IMPACT DYNAMICS
STATUS: READY
T+ 0.000s
FRAME: 0
Impact Parameters
Asteroid Diameter 500 m
Impact Velocity 20 km/s
Impact Angle 45°
Density 2500 kg/m³
Composition
Target World
🌍 Earth
🌕 Moon
🔴 Mars
🟡 Venus
⚪ Mercury
🟠 Jupiter
Surface Type
Quick Presets
Impact Analysis
THREAT CLASS
— AWAITING —
⬡ Impactor Properties
Diameter—
Mass—
Velocity—
Kinetic Energy—
TNT Equiv.—
◎ Crater Dimensions
Transient D—
Final Diameter—
Depth—
Ejecta Blanket—
Type—
⚡ Environmental Effects
Richter Equiv.—
Fireball Radius—
Blast Radius (5psi)—
Thermal Radius—
Peak Overpressure—
Ejecta Velocity—
🌊 Tsunami (ocean impacts)
Wave Height @100km—
Run-up Potential—
GLOBAL IMPACT SEVERITY0%
CRATER SIZE INDEX0%
Module Identity
Module IDAIS-NARROW-v2.1.0 © 2026 Astrophyzix
Display NameAsteroid Impact Simulator
Layout TargetNarrow / single-column ≤ 480 px
EngineHTML5 Canvas · Vanilla JS ES2020
Build Date2026-03-19
Status● ACTIVE
Physics Model Provenance
Crater ScalingHolsapple, K.A. (1993). The scaling of impact processes in planetary sciences. Ann. Rev. Earth Planet. Sci. 21, 333–373. Pi-group scaling laws; gravity & strength regime transitions.
Complex CratersMelosh, H.J. (1989). Impact Cratering: A Geologic Process. Oxford Univ. Press. Simple→complex transition diameter, depth/diameter ratios, central peak formation.
Environmental FXCollins, G.S., Melosh, H.J. & Marcus, R.A. (2005). Earth Impact Effects Program. Meteoritics & Planet. Sci. 40(6), 817–840. Seismic magnitude, blast radius, thermal radius.
Airburst ModelChyba, C.F., Thomas, P.J. & Zahnle, K.J. (1993). The 1908 Tunguska explosion. Nature 361, 40–44. Ram-pressure fragmentation altitude.
Ejecta / BlastGault, D.E. & Sonett, C.P. (1982). Laboratory simulation of pelagic asteroidal impact. GSA Spec. Paper 190. Ejecta blanket extent scaling.
TsunamiWeiss, R. & Wünnemann, K. (2008). Large waves from impact into shallow coastal water. AGU Monograph 174. Wave height at 100 km, run-up classification.
Atm. EffectsToon, O.B. et al. (1997). Environmental perturbations caused by the impacts of asteroids and comets. Rev. Geophys. 35(1), 41–78.
⚠ Simplifications applied: atmospheric deceleration uses single exponential scale-height; tsunami model assumes mean ocean depth 4 000 m; shock pressure uses first-order Hugoniot approximation. Results are order-of-magnitude estimates suitable for educational and scenario-planning purposes only. Do not use for hazard-assessment or civil-defence planning without validated simulation software.
Planetary Data Sources
PrimaryNASA Planetary Fact Sheets (Williams, D.R., NSSDCA) — surface gravity, escape velocity, mean atmospheric density, scale height, mean radius.
AtmosphereNSSDC / MSIS models for Earth; Mars Climate Database v6 for Mars; Venus VIRA for Venus; Jupiter Galileo probe entry data.
Last Verified2025-08
Material Parameter Provenance
Impactor DensityBritt, D.T. & Consolmagno, G.J. (2003). Stony meteorite porosities and densities. Meteoritics 38, 1161–1180.
Cometary NucleusA'Hearn, M.F. et al. (2011). EPOXI at comet Hartley 2. Science 332, 1396–1400. Bulk density ≈ 500 kg m⁻³.
Target Strength YtMelosh (1989) Table A.1; laboratory Hugoniot data for rock, soil, ice, and water.
Pi-group μ, K₁Holsapple (1993) Table 1; Schmidt & Housen (1987) experimental fits.
Known Limitations & Caveats
Oblique ImpactsAngle enters only via sin(θ) normal-velocity term. Real oblique impacts produce elliptical craters and asymmetric ejecta not modelled here.
Secondary CratersEjecta re-impact and secondary cratering field not computed.
FragmentationMulti-body fragmentation during entry not modelled; airburst treated as point source.
TsunamiFar-field propagation assumes flat-bottomed ocean; shoaling and run-up on real bathymetry not included.
JupiterNo solid surface; crater model applied to cloud-deck for illustrative purposes only.
Very Large EventsPi-group scaling breaks down above ~500 km crater diameter (Chicxulub scale); results are extrapolations.
Governance & Usage Policy
Intended UseEducation, science communication, scenario visualisation, and interactive demonstrations.
Prohibited UseOperational hazard assessment · insurance or liability claims · civil defence planning without independent verification.
Accuracy TierINDICATIVE — order-of-magnitude. Uncertainties typically ±50 % on crater dimensions, ±1 order of magnitude on energy effects.
Peer ReviewPhysics sourced from peer-reviewed literature; implementation not independently validated.
Change ControlVersion increments require review of affected physics modules. Breaking changes bump major version.
AccessibilityCanvas simulation has no screen-reader equivalent. All numerical results are available in the text panel.
EDUCATIONAL USE ✓
OPEN SOURCE
NOT FOR OPERATIONAL HAZARD USE
NO PERSONAL DATA COLLECTED
CLIENT-SIDE ONLY
Changelog
v2.1.0Narrow single-column layout rebuild. Canvas fixed-height scroll layout. Preset grid 2×2. Provenance drawer added.
v2.0.0Three-column desktop layout. Added airburst altitude model (Chyba 1993). Tsunami module (Weiss & Wünnemann 2008).
v1.0.0Initial release. Pi-group crater scaling, Holsapple (1993). Six planet targets. Canvas particle system.