# Toward a Population Synthesis of Disks and Planets I. Evolution of Dust with Entrainment in Winds and Radiation Pressure

**Authors:** Remo Burn, Alexandre Emsenhuber, Jesse Weder, Oliver Völkel, Hubert Klahr, Til Birnstiel, Barbara Ercolano, Christoph Mordasini  
**arXiv:** [2207.08600](https://arxiv.org/abs/2207.08600)  
**Date:** 2022-07-18  
**Summary page:** https://www.summarizepaper.com/en/paper/2207.08600v1/

## Key points

- The study focuses on the evolution of dust in planetary systems and its impact on planet formation.
- The authors investigate the effects of dust entrainment in photoevaporative winds and radiation pressure caused by the central star.
- They improved and extended an existing two-population dust and pebble description in a global Bern/Heidelberg planet formation and evolution model.
- Modern prescriptions for photoevaporative winds were used, accounting for settling and advection of dust when calculating entrainment rates.
- A wide range of disk-, photoevaporation-, and dust-parameters were explored to prepare for future population studies with varying conditions.
- If dust can grow to pebble sizes, drift dominates, resulting in small but larger entrained masses than under the assumption of no vertical advection of grains with gas flow.
- Fragile dust shatters at velocities of 1 m/s - as indicated in laboratory experiments - an order of magnitude more dust is entrained, becoming the main removal process.
- Radiation pressure effects disperse massive, dusty disks on timescales of a few hundred million years.
- Dust entrainment in winds is highlighted as a solid mass removal process during planet formation that needs to be considered.
- This model extension lays the foundation for future statistical studies of planet formation in their birth environment.
- Overall, this study provides valuable insights into how different factors affect the evolution of planetary systems' birthplaces.

## Summary

This study focuses on the evolution of dust in planetary systems and its impact on planet formation. The authors aim to investigate the effects of dust entrainment in photoevaporative winds and radiation pressure caused by the central star. To achieve this, they improved and extended an existing two-population dust and pebble description in a global Bern/Heidelberg planet formation and evolution model. They used modern prescriptions for photoevaporative winds and accounted for settling and advection of dust when calculating entrainment rates. The authors explored a wide range of disk-, photoevaporation-, and dust-parameters to prepare for future population studies with varying conditions. They found that if dust can grow to pebble sizes, drift dominates, resulting in small but larger entrained masses than under the assumption of no vertical advection of grains with gas flow. However, if fragile dust shatters at velocities of 1 m/s - as indicated in laboratory experiments - an order of magnitude more dust is entrained, becoming the main removal process. Radiation pressure effects disperse massive, dusty disks on timescales of a few hundred million years. These results highlight the importance of considering dust entrainment in winds as a solid mass removal process during planet formation. Furthermore, this model extension lays the foundation for future statistical studies of planet formation in their birth environment. Overall, this study provides valuable insights into how different factors affect the evolution of planetary systems' birthplaces. By improving our understanding of these processes, we can better compare theoretical models with observations and gain a deeper understanding of how planets form and evolve over time.