Consequences of tidal interaction between disks and orbiting protoplanets for the evolution of multi-planet systems with architecture resembling that of Kepler 444
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Abstract
We study orbital evolution of multi-planet systems with masses in the
terrestrial planet regime induced through tidal interaction with a
protoplanetary disk assuming that this is the dominant mechanism for producing
orbital migration and circularization. We develop a simple analytic model for a
system that maintains consecutive pairs in resonance while undergoing orbital
circularization and migration. Migration times for each planet may be estimated
once planet masses, circularization times and the migration time for the
innermost planet are given. We applied it to a model system with the current
architecture of Kepler 444 interacting with a protoplanetary disk, the
evolution time for the system as a whole being comparable to current
protoplanetary disk lifetimes.
In addition we performed numerical simulations with input data obtained from
this model. These indicate that although the analytic model is inexact,
relatively small corrections to estimated migration rates yield systems for
which period ratios vary by a minimal extent. Because of relatively large
deviations from exact resonance in the observed system of up to
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1572-9478