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E. J. Rivera (Carnegie Institution of Washington), J. J. Lissauer (NASA/Ames Research Center)
We present two planet fits to the radial velocity measurements of the M dwarf star GJ 876 that account for the mutual perturbations between the planets as well as their interactions with the star. Our Newtonian models fit the data much better than do Keplerian models, reducing the \chi\nu2 from 1.88 to as low as 1.34 for an unstable high-inclination system and 1.43 for a stable low-inclination system. Several different local minima with comparable \chi\nu2 are found in parameter space; so our results are not able to provide tight constraints on the inclinations of the orbits to the line of sight and actual planetary masses. Most sets of planetary parameters that we have derived represent systems that are stable for at least 100 Myr.
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Bulletin of the American Astronomical Society, 34, #3
© 2002. The American Astronomical Society.