Photoionization feedback in turbulent molecular clouds
arXiv:2011.00020 · doi:10.1093/mnras/staa3380
Abstract
We present a study of the impact of photoionization feedback from young massive stars on the turbulent statistics of star-forming molecular clouds. This feedback is expected to alter the density structure of molecular clouds and affect future star formation. Using the AMUN- Rad code, we first generate a converged isothermal forced turbulent density structure inside a periodic box. We then insert an ionizing source in this box and inject photoionization energy using a two-temperature pseudo-isothermal equation of state. We study the impact of sources at different locations in the box and of different source luminosities. We find that photoionization has a minor impact on the 2D and 3D statistics of turbulence when turbulence continues to be driven in the presence of a photoionizing source. Photoionization is only able to disrupt the cloud if the turbulence is allowed to decay. In the former scenario, the presence of an HII region inside our model cloud does not lead to a significant impact on observable quantities, independent of the source parameters.
10 pages, 7 figures
References in corpus (12)
- Theory of Star Formation
- What determines the density structure of molecular clouds ? A case study of Orion B with Herschel
- On the Density Distribution in Star-forming Interstellar Clouds
- Before the first supernova: combined effects of HII regions and winds on molecular clouds
- Turbulence and star formation efficiency in molecular clouds: solenoidal versus compressive motions in Orion B
- Turbulence in the Interstellar Medium
- Power-law tails in probability density functions of molecular cloud column density
- Molecular Cloud Turbulence and Star Formation
- The onset of large scale turbulence in the interstellar medium of spiral galaxies
- Deciphering the 3-D Orion Nebula-I: Expanding Shells in the Huygens Region
- CMacIonize 2.0: a novel task-based approach to Monte Carlo radiation transfer
- The Density Variance--Mach Number Relation in Supersonic Turbulence: I. Isothermal, magnetised gas