HIGHTISTIC (Russell Vernon Trent III) · SNSFT Foundation uuia.app/galaxy · [9,9,9,9]
SHOTS
Rate8 shots/s
Spawn
GENERATOR
Band mix %
Noble
Locked
IVA
Shatter
Radius from
FIELD
Arms
Pitch angle20°
Time rate×1
GRAVITY · SELF-PULL + FUSION
Stars pull on each other (Newton's G, masses from the measured disk Σ(R)) and move freely. The rotation curve fixes the mean pull; self-gravity adds the local lumps. Two stars fuse by the GAMCollider 2-beam rule [9,9,2,3.8] only where they are close, bound, approaching, and their neighbourhood is gravitationally unstable (local Toomre Q < 1, measured live from the stars in each 2 kpc cell), the standard sink-particle criteria.
Fusion: P = P₁P₂/(P₁+P₂) · N = N₁+N₂ · B = |B₁−B₂| · A = max(A₁,A₂). Mass and momentum are conserved. A product with τ ≥ TL shatters and is ejected.
τ MODEL
Boundary identification: Toomre Q = 1 (disk breaks into clumps) ↔ τ = TL. Each settled star takes τ = TL/Q at its radius; B = τ × P.
Σ(R₀) M☉/pc²
σR(R₀) km/s
Rd kpc
VIEW
Drag to turn, scroll to zoom. TOP is the best angle for spirals.
SAG A*
TORSION τ = B/P
Noble 0LockedIVA≥ TL
PHASE MIX
± is two standard errors of a proportion, 2√(p(1−p)/n). The chip reads WITHIN when the observed share sits inside that band. Shots count when they settle; Shatter shots fly slower, so their share lags until a run has landed.
Largest clumps with their radius, member count, accumulated Narrative N, torsion τ/TL and the disk's local Toomre Q at that radius.
LIVE PHASES · τ = TL/Q
Q(R) = σRκ / (3.36 G Σ) (Toomre 1964). κ from the rotation curve; Σ ∝ e−R/Rd; σR ∝ e−R/2Rd. Dashed line: Q = 1, which is τ = TL.
RADIAL PHASE PROFILE
ROTATION CURVE
v(R) = vflat · R / √(R² + Rc²): rising through the center, flat outside, the measured shape of disk-galaxy rotation curves. Speed in km/s against radius in kpc, scaled to vflat = Θ₀ = 238 km/s with the Sun at R₀ = 8.2 kpc (Bland-Hawthorn & Gerhard 2016).