Moon Formation via DRUMS Superfluid–Substrate Dynamics

1. Failure of Impact Composition Constraint

The Moon exhibits near-identical isotopic composition to Earth's mantle:

\[ \delta^{17}O_{\oplus} \approx \delta^{17}O_{\text{Moon}} \]

Any viable model must produce material sourced primarily from Earth's mantle, not an external body.

2. DRUMS Rotating Superfluid Earth

Model early Earth as a rotating superfluid mass coupled to a cubic substrate. The velocity field is:

\[ \mathbf{v} = \frac{\hbar}{m} \nabla \theta + \mathbf{\Omega} \times \mathbf{r} \]

Where \(\Omega\) is planetary rotation. This produces quantized vortex structures.

3. Vortex-Induced Mass Ejection

Energy density in rotating superfluid:

\[ E = \int \left( \frac{1}{2} \rho |\mathbf{v}|^2 + \gamma |\nabla^2 h|^2 \right) dV \]

At critical rotation, centrifugal and surface tension terms produce instability:

\[ \rho \Omega^2 r \sim \frac{\gamma}{r^3} \]

Solving for critical radius:

\[ r_c \sim \left( \frac{\gamma}{\rho \Omega^2} \right)^{1/4} \]

This defines the radius at which material is preferentially ejected.

4. Harmonic Orbital Stabilization

Once ejected, material settles into DRUMS harmonic orbital modes:

\[ r_n^3 = n C \]

Where \(C\) is determined by system angular momentum:

\[ C \sim \frac{L}{\rho_{sf}} \]

This produces discrete stable radii independent of collision dynamics.

5. Angular Momentum Conservation

Total system angular momentum:

\[ L = I_{\oplus} \Omega + m_{\text{moon}} \sqrt{G M_{\oplus} r} \]

In DRUMS, allowed states correspond to quantized solutions of:

\[ \Delta L = n \hbar_{\text{eff}} \]

Ensuring stable Earth–Moon configuration without fine-tuned impact parameters.

6. Composition Result

7. Testable Predictions

8. Conclusion