摘要：I will go through the solar system formation history with two important phenomena: the NC/CC meteorite dichotomy and the giant planet's dynamical instability. Meteorites display an isotopic composition dichotomy between non-carbonaceous (NC) and carbonaceous (CC) groups. This indicates that planetesimal formation in the solar protoplanetary disk occurred in two distinct reservoirs over the first several Myr. I will introduce an expanding disk model to explain the long separation of these two disk reservoirs. Meanwhile, the four giant planets in our solar system are thought to be migrated and trapped into a compact, resonant chain during the gas-rich disk phase. Our work supports that the giant planets’ dynamical instability was likely triggered by the inside-out dispersal of the gaseous disk, constrained to be a few to ten million years after the birth of the solar system.