HIGHTISTIC (Russell Vernon Trent III) · SNSFT Foundation uuia.app/accretion · [9,9,9,9]
SYSTEM
Speed (compute per frame)10 ms
DISK · MINIMUM MASS SOLAR NEBULA
Planetesimals200
Radius enhancement f (resolution)×100
Σ₁ solids at 1 AU, g/cm²
× beyond snow line (2.7 AU)
Σ(r) = Σ₁ (r / 1 AU)−3/2, the Minimum Mass Solar Nebula (Weidenschilling 1977; Hayashi 1981). Equal-mass bodies, rock 3 g/cm³ inside the snow line, ice-rock 1.5 g/cm³ beyond. Disk settings apply on ⟲ NEW RUN.
f multiplies every collision radius, the standard way to fit accretion into a short run (Kokubo & Ida 1996 used f = 5–6). Growth runs faster by roughly f, so read the clock as compressed by about that factor. Gravity, orbits and the collision physics are unchanged.
τ MODEL
Band mix % at birth
Noble
Locked
IVA
Shatter
Merger product by the 2-beam rule of the GAM Collider v15 (Geometric Axiomatic Module Collider) [9,9,2,3.8]: P = P₁P₂/(P₁+P₂) · N = N₁+N₂ · B = |B₁−B₂| · A = max(A₁,A₂). A body with τ ≥ TL reorganizes: it splits into two halves with P doubled and N halved (each half carries τ/2), repeated until each piece sits below TL. Mass and momentum are conserved.
COLLISIONS
Two bodies that touch merge if the impact is slow enough, otherwise they glance off each other (hit-and-run). The dividing speed vcr comes from the collision simulations of Kokubo & Genda (2010) and depends on the mass ratio and the impact angle. Boundary identification: τc = TL × vimp / vcr, so a collision merges below TL and hits and runs at or above it.
vcr/vesc = 2.43Γ²Θ5/2 − 0.0408Γ + 1.86Θ5/2 + 1.08, Γ = (M₁−M₂)/(M₁+M₂), Θ = 1 − sin θ. vesc = √(2G(M₁+M₂)/(R₁+R₂)) with physical radii; vimp = √(v∞² + vesc²), v∞ taken from the encounter at the enhanced contact distance.
VIEW
Drag to turn, scroll to zoom. Bright flashes are collisions: teal-to-gold flashes merged, red flashes hit and ran.
Disk view is linear, 40 scene units per AU, heights ×4. Solar System view compresses distance as 60√(r/AU) so Mercury and Neptune fit together. Body size grows as the cube root of mass.
SUN
SNOW LINE 2.7 AU
TORSION τ = TL × 2√3 / Δ
Noble 0LockedIVA≥ TL
0 yrorbits at 1 AU
SYSTEM
Bodies0
Largest masses (M⊕)—
Isolation mass at 1 AU—
Total mass in bodies—
Merged · hit-and-run0 · 0
Fragments · lost to Sun · ejected0 · 0 · 0
PHASE MIX
HILL SPACING · τ = TL × 2√3 / Δ
GROWTH
White: number of bodies. Gold: largest mass in M⊕. Dashed: isolation mass at 1 AU. Both axes in log scale; time in years (compressed by about f).
MASS AGAINST ORBIT
IMPACTS · τc = TL × vimp/vcr
Every collision so far, binned by τc/TL. Left of the line merged; right of it hit and ran.