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PRODID:-//Heidelberg University//HePhySTO//EN
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DTEND:20260428T153000Z
UID:4848f213b30a0a12d2be915bdcbe3cc2@physik.uni-heidelberg.de
DTSTAMP:20260411T181113Z
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DESCRIPTION:Well-characterised multiple-exoplanet systems are particularly 
 valuable because their physical and dynamical architectures preserve a foss
 il record of their formation and subsequent dynamical evolution. In strongl
 y interacting systems composed of massive Jovian planets detected through r
 adial velocities (RVs) and transit timing variations (TTVs)\, the mutual gr
 avitational interactions are strong enough to constrain the system architec
 ture with high precision through N-body dynamical modelling. Such models re
 cover the time-dependent osculating orbital elements that more accurately d
 escribe the true configuration and dynamical state of the system.\nReproduc
 ing the observed dynamical architecture of these systems enables reverse en
 gineering of the initial conditions under which they formed. In particular\
 , planetary systems trapped in mean-motion resonances (MMRs) retain a “memo
 ry” of the migration process\, including the possible migration rate during
  the proto-planetary disk phase\, the excitation of eccentricity\, and disk
 -planet interactions at the moment of capture. In this talk\, I will presen
 t the cascade from observations to detailed dynamical modelling of the data
 \, and the following migration simulations. I will highlight several except
 ionally well-characterised giant planet systems that provide important insi
 ghts into the mechanisms shaping planetary systems during their formation a
 nd early evolution.\n\nImported from https://www.physik.uni-heidelberg.de/h
 ephysto/ (no warranty for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=12463
SUMMARY:Heidelberg Joint Astronomical Colloquium: Trifon Triofnov  - Strong
 ly Interacting Multiple Planet Systems as a Rosetta Stone for Planet Format
 ion
DTSTART:20260428T143000Z
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