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We use the super Earth 55 Cnc e as a case study to address an observableeffect of tidal heating. We investigate whether planet-planet interactions canforce the eccentricity of this planet to a level affecting the eclipse depthobserved with Spitzer. Using the constant time lag tidal model, we firstcalculate the observed planet flux as a function of albedo and eccentricity,for different tidal dissipation constants and for two extreme cases: a planetwith no heat redistribution and a planet with full heat redistribution. Wederive the values of albedo and eccentricity that match the observed transitdepth. We then perform N-body simulations of the planetary system includingtides and General Relativity to follow the evolution of the eccentricity ofplanet e. We compare the range of eccentricities given by the simulations withthe eccentricities required to alter the eclipse depth. We find that theeccentricity of planet e can be large enough to contribute at a measurablelevel to the thermal emission measured with Spitzer. This affects theconstraints on the albedo of the planet, which can be as high as 0.9 (insteadof 0.55 when ignoring tidal heating). We also derive a maximum value for theeccentricity of planet e directly from the eclipse depth: e<0.015 assumingEarth's dissipation constant. Transiting exoplanets in multiple planet systemsare exceptional targets for testing tidal models because their tidal luminositymay be observable. Future multi-wavelengths observations of eclipse depth andphase curves (for instance with EChO and JWST) should allow us to betterresolve the temperature map of these planets and break the degeneracy betweenalbedo and tidal heating that remains for single band observations. Inaddition, an accurate determination of the eccentricity will make it possibleto constrain the dissipation rate of the planet and to probe its internalstructure.

Tidal dissipation and eccentricity pumping: Implications for the depth of the secondary eclipse of 55 Cnc e