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    Re: Oblateness calculation given observer's latitude
    From: Peter Monta
    Date: 2018 Feb 5, 09:03 -0800
    Frank writes:

    > And you'll always get values in the lowest lying members of the sequence (like J2) in a lumpy body like the Moon, even if it's not by itself much use in describing the Moon's shape.

    There's some discussion in this Clementine paper:


    Figure 10 seems to show that the ellipsoid is real but weak.  The polar and equatorial radii differ by 2 km, and the detailed topography accounts for the remaining 2 km rms (figure 8).  The ellipticity seems reasonably robust to model order.  Figure 11 shows the center-of-figure offsets.

    It seems doubtful that the ellipsoid is of much use as a simple intermediate step prior to accounting for the detailed topography.  Taking out only half the error, the ellipsoid is not exactly covering itself in glory.

    > [ long-wavelength gravity terms, pear shape, J3 ]
    > That early space age description is a mathematical artifact with little physical meaning.

    Long-wavelength terms do have a disproportionate impact on orbits, though.  High-order tidal terms peter out very rapidly, but the low-order ones more slowly, so they dominate for high orbits.  Ultimately it's only the dipole that matters (and then, if you're really far out, the monopole).  So a satellite sees a pear-shaped Earth in a physically meaningful way, but humans have to squint.  (Well, J3 is on the same order as the low-order tesseral terms, so it's the overall "low-order lumpiness", not a distinct pear.)

    I'm still waiting for the super-sextant that I can wave in the general direction of the Moon, from a moving platform, and get arcsecond offsets to the stars.  Then there will be a cry for better lunar models in the reduction software.


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