When we think about finding extra-solar planets from the reflex motions they imprint into stellar radial-velocity data, we think about the problem of noise: There is shot noise, there are spectrograph-calibration offsets, there are imprints of the atmosphere, there is surface convection on the star and asteroseismic modes, there is magnetic activity, flaring, and so on! It's a mess. But there's also noise from other, unmodeled and undiscovered planets. That is, the other things orbiting the star, other than the planet of interest.
Today, Winston Harris (MTSU), Megan Bedell (Flatiron) and I came up with a plan for inserting this planetary-system noise into Harris's simulations of radial-velocity data. The question arose: What periods to use for the planets? And Bedell suggested that we adapt the Titius–Bode law! Hilarious. This gives us an extra-solar system architecture that makes sense, and simultaneously trolls anyone reading our paper.
[Insert here obligatory objection to naming things after people.]
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