Pulse Core Lexicon
Gas Depletion Law
Definition
The Gas Depletion Law is how fast a universe's gas turns into stars: t⇣⊛ = t⇣⊚ · (ρ / ρ⇥)^(−0.4), a depletion time shorter where the gas is denser, the Kennicutt–Schmidt law written as a time (Kennicutt 1998; Bigiel et al. 2008). At the threshold density ρ⇥ the time is t⇣⊚, about 2 × 10⁹ years in galaxies today, 0.145 of the universe's life; it is the rule every simulation of a universe uses below the scale it can resolve, since none resolves the cores where stars form. The game applies it to every cloud of gas denser than twice the mean (stars.js). It connects to Depletion Time Evolution, Star Formation Condition, Solar Mass of a Universe and Stellar Mass Unit.
Mathematical Expression
From the book · Chapter 6 · Stellar Formalism: The Gas, the Stellar Mass Unit, and the Stellar Null Well
t⇣⊛ = t⇣⊚ · (ρ / ρ⇥)^(−0.4)
Dimensional analysis:
Where (from the book): t⇣⊛ [𝕋], t⇣⊚ [𝕋], ρ [𝕄·𝕃⁻³], ρ⇥ [𝕄·𝕃⁻³]
[𝕋]
[𝕋] × ([𝕄·𝕃⁻³] ÷ [𝕄·𝕃⁻³])^([∅]) = [𝕋] × ([𝕄·𝕃⁻³] ÷ [𝕄·𝕃⁻³])^([∅]) = [𝕋] × [∅]^([∅]) = [𝕋] × [∅] = [𝕋]
[𝕋] = [𝕋] ✓ Valid PulseCore Verified ✓
Gas in galaxies turns into stars over a depletion time, shorter where it is denser
Where:
- t⇣⊛ [𝕋] — the time a region takes to turn its gas into stars at its present rate
- t⇣⊚ [𝕋] — the depletion time at the threshold density: about 2 × 10⁹ years in galaxies today, about 0.145 of the universe's age
- ρ [𝕄·𝕃⁻³] — the density of the gas
- ρ⇥ [𝕄·𝕃⁻³] — the threshold above which gas forms stars
Technical Details
Category Law
Chapter Chapter 6
Importance
In the book #413 of 1,287 terms · used 3 times