Modelling of ionizing feedback with smoothed particle hydrodynamics and Monte Carlo radiative transfer on a Voronoi grid

• Verfasst von: Petkova, Maya A. [VerfasserIn]
• Verfasst von: Vandenbroucke, Bert [VerfasserIn]
• Verfasst von: Bonnell, Ian [VerfasserIn]
• Verfasst von: Kruijssen, Diederik [VerfasserIn]
• Titel: Modelling of ionizing feedback with smoothed particle hydrodynamics and Monte Carlo radiative transfer on a Voronoi grid
• Verf.angabe: Maya A. Petkova, Bert Vandenbroucke, Ian A. Bonnell and J.M. Diederik Kruijssen
• E-Jahr: 2021
• Jahr: 2021 July 31
• Umfang: 21 S.
• Fussnoten: Gesehen am 01.04.2022
• Titel Quelle: Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society
• Ort Quelle: Oxford : Oxford Univ. Press, 1827
• Jahr Quelle: 2021
• Band/Heft Quelle: 507(2021), 1 vom: Okt., Seite 858-878
• ISSN Quelle: 1365-2966
• DOI: doi:10.1093/mnras/stab2178
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 1776044770

Abstract

The ionizing feedback of young massive stars is well known to influence the dynamics of the birth environment and hence plays an important role in regulating the star formation process in molecular clouds. For this reason, modern hydrodynamics codes adopt a variety of techniques accounting for these radiative effects. A key problem hampering these efforts is that the hydrodynamics are often solved using smoothed particle hydrodynamics (SPH), whereas radiative transfer is typically solved on a grid. Here we present a radiation-hydrodynamics (RHD) scheme combining the SPH code phantom and the Monte Carlo radiative transfer (MCRT) code cmacionize, using the particle distribution to construct a Voronoi grid on which the MCRT is performed. We demonstrate that the scheme successfully reproduces the well-studied problem of D-type H ii region expansion in a uniform density medium. Furthermore, we use this simulation setup to study the robustness of the RHD code with varying choice of grid structure, density mapping method, and mass and temporal resolution. To test the scheme under more realistic conditions, we apply it to a simulated star-forming cloud reminiscing those in the Central Molecular Zone of our Galaxy in order to estimate the amount of ionized material that a single source could create. We find that a stellar population of several $10^3~\rm {M_{\odot }}$ is needed to noticeably ionize the cloud. Based on our results, we formulate a set of recommendations to guide the numerical setup of future and more complex simulations of star forming clouds.