CHPS Seminar | Reconstructing the properties of the protosolar disk using cosmochemistry

Observations of protoplanetary disks with ALMA have revealed a large diversity of properties, but also some common tendencies in terms of dust/gas density and radial extension ratios, as well as the appearance of features like rings and gaps or cavities. It is too late to observe the proto-solar disk, but many of its properties can be inferred from the current distribution of planetesimals and using cosmochemical constraints on the chronology of planetesimal accretion and the isotopic heterogeneity of the disk. I will review the available data, which can be used to reconstruct the proto-solar disk. The view that emerges is that of a quite standard disk of about 90 au in gas radius and 45 au in dust radius, forming planetesimals at two distinct epochs (one of which is very early, while the disk was presumably still in Class-0 or Class-1 stage) and evolving towards a transition disk at the appearance of Jupiter and Saturn. Similarities and differences with the PDS70 disk will be discussed.