The classical model for the formation of the Solar System invokes the gravitational collapse of a cold molecular cloud of interstellar gas, its heating, and the formation of a central star (Lewis 1995; Pfalzner et al. 2015). A flattened spinning protoplanetary disk of dust and gas surrounding the protosun extends for 100 AU (1AU ≈ Earth to Sun distance ≈ 150 × 106 km). Initially hot, this disk later cools down (T-Tauri stage). Since the heat flux is greatest close to the sun and at places where the cloud is the densest, the disk is hotter...

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