English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Ionising feedback from massive stars dramatically affects the interstellarmedium local to star forming regions. Numerical simulations are now starting toinclude enough complexity to produce morphologies and gas properties that arenot too dissimilar from observations. The comparison between the density fieldsproduced by hydrodynamical simulations and observations at given wavelengthsrelies however on photoionisation/chemistry and radiative transfercalculations. We present here an implementation of Monte Carlo radiationtransport through a Voronoi tessellation in the photoionisation and dustradiative transfer code MOCASSIN. We show for the first time a syntheticspectrum and synthetic emission line maps of an hydrodynamical simulation of amolecular cloud affected by massive stellar feedback. We show that the approachon which previous work is based, which remapped hydrodynamical density fieldsonto Cartesian grids before performing radiative transfer/photoionisationcalculations, results in significant errors in the temperature and ionisationstructure of the region. Furthermore, we describe the mathematical process oftracing photon energy packets through a Voronoi tessellation, includingoptimisations, treating problematic cases and boundary conditions. We performvarious benchmarks using both the original version of MOCASSIN and the modifiedversion using the Voronoi tessellation. We show that for uniform grids, orequivalently a cubic lattice of cell generating points, the new Voronoi versiongives the same results as the original Cartesian-grid version of MOCASSIN forall benchmarks. For non-uniform initial conditions, such as using snapshotsfrom Smoothed Particle Hydrodynamics simulations, we show that the Voronoiversion performs better than the Cartesian grid version, resulting in muchbetter resolution in dense regions.

Observing gas and dust in simulations of star formation with Monte Carlo radiation transport on Voronoi meshes