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While about a dozen transiting planets have been found in wide orbits aroundan inner, close stellar binary (so-called "P-type planets"), no planet has yetbeen detected orbiting only one star (a so-called "S-type planet") in aneclipsing binary. This is despite a large number of eclipsing binary systemsdiscovered with the Kepler telescope. Here we propose a new detection methodfor these S-type planets, which uses a correlation between the stellar radialvelocities (RVs), eclipse timing variations (ETVs), and eclipse durationvariations (EDVs). We test the capability of this technique by simulating arealistic benchmark system and demonstrate its detectability with existinghigh-accuracy RV and photometry instruments. We illustrate that, with a smallnumber of RV observations, the RV-ETV diagrams allows us to distinguish betweenprograde and retrograde planetary orbits and also the planetary mass can beestimated if the stellar cross-correlation functions can be disentangled. Wealso identify a new (though minimal) contribution of S-type planets to theRossiter-McLaughlin effect in eclipsing stellar binaries. We finally explorepossible detection of exomoons around transiting luminous giant planets andfind that the precision required to detect moons in the RV curves of their hostplanets is of the order of ${\rm cm\,s}^{-1}$ and therefore not accessible withcurrent instruments.

How eclipse time variations, eclipse duration variations, and radial velocities can reveal S-type planets in close eclipsing binaries