We analyse the Transit Timing Variation ( TTV ) measurements of a system of two super-Earths detected as Kepler-29 , in order to constrain the planets ’ masses and orbital parameters .
A dynamical analysis of the best-fitting configurations constrains the masses to be \sim 6 and \sim 5 Earth masses for the inner and the outer planets , respectively .
The analysis also reveals that the system is likely locked in the 9:7 mean motion resonance .
However , a variety of orbital architectures regarding eccentricities and the relative orientation of orbits is permitted by the observations as well as by stability constraints .
We attempt to find configurations preferred by the planet formation scenarios as an additional , physical constraint .
We show that configurations with low eccentricities and anti-aligned apsidal lines of the orbits are a natural and most likely outcome of the convergent migration .
However , we show that librations of the critical angles are not necessary for the Kepler-29 system to be dynamically resonant , and such configurations may be formed on the way of migration as well .
We argue , on the other hand , that aligned configurations with e \gtrsim 0.03 may be not consistent with the migration scenario .