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Since exoplanets were detected using the radial velocity method, they haverevealed a diverse distribution of orbital configurations. Amongst these areplanets in highly eccentric orbits (e > 0.5). Most of these systems consist ofa single planet but several have been found to also contain a longer periodplanet in a near-circular orbit. Here we use the latest Keplerian orbitalsolutions to investigate four known systems which exhibit this extremeeccentricity diversity; HD 37605, HD 74156, HD 163607, and HD 168443. We placelimits on the presence of additional planets in these systems based on theradial velocity residuals. We show that the two known planets in each systemexchange angular momentum through secular oscillations of their eccentricities.We calculate the amplitude and timescale for these eccentricity oscillationsand associated periastron precession. We further demonstrate the effect ofmutual orbital inclinations on the amplitude of high-frequency eccentricityoscillations. Finally, we discuss the implications of these oscillations in thecontext of possible origin scenarios for unequal eccentricities.

Orbital Dynamics of Multi-Planet Systems with Eccentricity Diversity