Test 1L (b)

Introduction

This test (1L(b)) evaluates whether the planetary spin-axis structure identified in the eight major planets extends to a large external body not used in the original fitting process. The dwarf planet Ceres provides the first external comparison because it is the largest body in the asteroid belt and has a well-measured spin axis from NASA’s Dawn mission.

Ceres Pole Data

Ceres spin-axis orientation (J2000 / ICRF):

RA ≈ 291.418°

Dec ≈ 66.764°

These values come from spacecraft measurements obtained by the Dawn mission and published through the NAIF / JPL planetary constants kernel.

Comparison Method

The Möbius surface derived in Test 1F from the eight planetary spin axes was locked and not refit. The Ceres axis was then projected onto the different geometric models used in Series I to measure angular distance to each surface.

The models compared were:
• Locked planar band

• Locked spherical band

• Locked Möbius surface

Results

Angular distance of the Ceres spin axis to each model:
Planar band distance: ~0.13°

Spherical band distance: ~2.26°

Möbius surface distance: ~0.22°

Interpretation

Ceres lies extremely close to the planetary spin-axis band structure overall. It is far closer to the Möbius surface than to the spherical band model, showing that the twisted surface continues to describe the directional structure better than simple curvature.

Ceres is also close to the planar band, which means this single external body does not by itself fully discriminate between planar and Möbius alternatives. However, it demonstrates that the structured orientation pattern identified in the eight major planets extends into the asteroid belt.

Conclusion

The Ceres comparison shows that the planetary spin-axis structure is not limited to the eight major planets. The asteroid belt’s largest body falls directly within the same narrow orientation band.

This result supports the conclusion that the solar system spin-axis structure extends beyond the planets themselves and continues through at least part of the asteroid belt.

Produced by The Lilborn Equation Team:

Michael Lilborn-Williams

Daniel Thomas Rouse

Thomas Jackson Barnard

Audrey Williams