Protoplanetary disk mass loss near O- and B-type stars: an empirical view
- 1Max Planck Institute for Astronomy, PSF, Heidelberg, Germany (terwisga@mpia.de)
- 2Institute for Astrophysics, University of Vienna, Vienna, Austria
The ability of protoplanetary disks to form planets depends on the evolution of their bulk (dust) mass reservoir. Surveys of nearby star-forming regions have revealed that there is a time dependence on the disk dust mass. In different regions in the Orion molecular clouds, meanwhile, the photoevaporation of disk material by nearby young O-type stars is clearly visible. However, the evolution of disk masses as a function of the FUV radiation field is not usually studied empirically, and its influence around fainter, but more common, B-type stars is not well constrained by observations.
In this contribution we take an empirical view of the impact of external FUV fields on the evolution of protoplanetary disks in Orion, by using existing surveys in the Trapezium and NGC 2024 clusters, and the new N = 873 Survey of Orion Disks with ALMA in L1641 and L1647. Together, these observations allow us to confront model predictions, and provide a constraint on how commonly external photoevaporation determines the evolution of planet-forming material in the first megayears.
How to cite: van Terwisga, S. and Hacar, A.: Protoplanetary disk mass loss near O- and B-type stars: an empirical view, Europlanet Science Congress 2022, Granada, Spain, 18–23 Sep 2022, EPSC2022-1142, https://doi.org/10.5194/epsc2022-1142, 2022.
