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Five planets are known to orbit the star 55 Cancri. The recently-discoveredplanet f at 0.78 AU (Fischer et al. 2008) is located at the inner edge of apreviously-identified stable zone that separates the three close-in planetsfrom planet d at 5.9 AU. Here we map the stability of the orbital space betweenplanets f and d using a suite of n-body integrations that include anadditional, yet-to-be-discovered planet g with a radial velocity amplitude of 5m/s (planet mass = 0.5-1.2 Saturn masses). We find a large stable zoneextending from 0.9 to 3.8 AU at eccentricities below 0.4. For each system wequantify the probability of detecting planets b-f on their current orbits givenperturbations from hypothetical planet g, in order to further constrain themass and orbit of an additional planet. We find that large perturbations areassociated with specific mean motion resonances (MMRs) with planets f and d. Weshow that two MMRs, 3f:1g (the 1:3 MMR between planets g and f) and 4g:1dcannot contain a planet g. The 2f:1g MMR is unlikely to contain a planet moremassive than about 20 Earth masses. The 3g:1d and 5g:2d MMRs could contain aresonant planet but the resonant location is strongly confined. The 3f:2g,2g:1d and 3g:2d MMRs exert a stabilizing influence and could contain a resonantplanet. Furthermore, we show that the stable zone may in fact contain 2-3additional planets, if they are ~50 Earth masses each. Finally, we show thatany planets exterior to planet d must reside beyond 10 AU.

A dynamical perspective on additional planets in 55 Cancri