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 (42)
- Theory of Star Formation
- Control of star formation by supersonic turbulence
- The Star Formation Rate of Turbulent Magnetized Clouds: Comparing Theory, Simulations, and Observations
- The Universality of the Stellar IMF
- Probing the evolution of molecular cloud structure: From quiescence to birth
- Density probability distribution in one-dimensional polytropic gas dynamics
- Massive stars in massive clusters II: Disruption of bound clusters by photoionization
- 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
- Modeling UV Radiation Feedback from Massive Stars: II. Dispersal of Star-Forming Giant Molecular Clouds by Photoionization and Radiation Pressure
- Dispersal of molecular clouds by ionising radiation
- Characterizing the properties of nearby molecular filaments observed with Herschel
- The "True" Column Density Distribution in Star-Forming Molecular Clouds
- Dynamical Expansion of Ionization and Dissociation Front around a Massive Star. II. On the Generality of Triggered Star Formation
- A General Theory of Turbulent Fragmentation
- The density variance -- Mach number relation in supersonic, isothermal turbulence
- Dynamical HII Region Evolution in Turbulent Molecular Clouds
- Escape of Ionizing Radiation from High-Redshift Galaxies
- Turbulence and star formation efficiency in molecular clouds: solenoidal versus compressive motions in Orion B
- StarBench: The D-type expansion of an HII region
- Statistics of Reconnection-Driven Turbulence
- Ion-neutral friction and accretion-driven turbulence in self-gravitating filaments
- Photoionisation Feedback in a Self-Gravitating, Magnetised, Turbulent Cloud
- Outflow Driven Turbulence in Molecular Clouds
- Turbulence in the Interstellar Medium
- A 3D Monte Carlo Photoionization Code for Modeling Diffuse Ionized Gas
- The Lognormal Probability Distribution Function of the Perseus Molecular Cloud: A Comparison of HI and Dust
- Fervent: Chemistry-coupled, ionising and non-ionising radiative feedback in magnetohydrodynamical simulations
- Impact of Winds from Intermediate-Mass Stars on Molecular Cloud Structure and Turbulence
- Star Cluster Formation and Feedback
- Star Formation in Molecular Clouds
- Modelling massive-star feedback with Monte Carlo radiation hydrodynamics: photoionization and radiation pressure in a turbulent cloud
- Power-law tails in probability density functions of molecular cloud column density
- Turbulence in collisionless plasmas: statistical analysis from numerical simulations with pressure anisotropy
- The onset of large scale turbulence in the interstellar medium of spiral galaxies
- Molecular Cloud Turbulence and Star Formation
- A Markov model for non-lognormal density distributions in compressive isothermal turbulence
- The classical D-type expansion of spherical H II regions
- 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
Cited by in corpus (5)
- The formation of massive stellar clusters in converging galactic flows with photoionisation
- The growth of H II regions around massive stars: the role of metallicity and dust
- Stellar winds and photoionization in a spiral arm
- Modelling of ionising feedback with Smoothed Particle Hydrodynamics and Monte Carlo Radiative Transfer on a Voronoi grid
- Dust destruction by the supernova remnant forward shock in a turbulent interstellar medium