Speaker
Description
Given the variety of properties found in planetary systems in our Galaxy, we must analyse general disk and host star properties measured in a large statistical sample of systems at different evolutionary stages and environments. Disks in nearby regions evolve differently than disks in highly irradiated environments. Since the majority of (exo)planet host stars (including our Solar System) form in dense and massive stellar clusters in which the presence of OB-type stars dominates the radiation field, disk evolution studies must consider internal as well as external factors shaping the evolutionary path of protoplanetary disks in a complementary way.
During this talk, I will focus first on how the most “typical” disks in nearby regions look in dust continuum emission. Then, I will contrast these results with those found in a more representative cluster in Orion.
I will show the results of dust continuum analysis of 80 disks in 4 nearby star-forming regions as part of the DECO ALMA large program. I will present dust disk size estimates and dust morphology identification results obtained through visibility fitting with GALARIO. In contrast, I will also describe how disk evolution is affected by the feedback from massive OB stars in more distant clusters, focusing on the more representative sigma-Orionis cluster, where its innermost regions are clearly affected by external irradiation from the massive system sigma-Ori, suggesting a coevolution of internal and external winds in these disks.
| Category | Disk evolution and population (theory and observations) |
|---|---|
| Please don't forget to register for the event in addition to submitting your abstract. | I understand |