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The evolution of the mutual inclination on the same timescale as Figure 9.

The majority of the matter is ejected from the inner binary, and the inner binary shrinks moderately to weakly with (alphalambda_{mathrm{ce}} gtrsim3) depending on the mutual inclination of the system.

Simulations suggest that the mean mutual inclinations of the planetary orbits are about 1°, meaning the system is probably more coplanar (flatter) than the Solar System, where the corresponding figure is 2.3°.

Figures 3 and 4 show the evolution of the inner eccentricity and mutual inclination for the first 3 Myr after the birth of the system.

The dimensionless quantity α depends weakly on the mutual inclination, and on the eccentricity and argument of periastron of the inner binary, and is of order unity (Antognini 2015).

The change in the mutual inclination in Eq. (39) is based on the conservation of total angular momentum (Hamers et al. 2013).

Figure 4 Mutual inclination evolution.

As a result, the amplitudes of the cycles in inner eccentricity and mutual inclination are reduced.

As a consequence, the orbital inner eccentricity and mutual inclination vary periodically.

The evolution of the mutual inclination i as a function of time for the same triple as in Figure 13.

Parameters for the inner and outer orbit are denoted with a subscript 'in' and 'out', respectively; the mutual inclination (i_{r}) between the two orbits.