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

I review recent results derived from numerical simulations of the turbulent interstellar medium (ISM), in particular concerning the nature and formation of turbulent clouds, methods for comparing the structure in simulations and observations, and the effects of projection of three-dimensional structures onto two dimensions. Clouds formed as turbulent density fluctuations are probably not confined by thermal pressure, but rather their morphology may be determined by the large-scale velocity field. Also, they may have shorter lifetimes than normally believed, as the large-scale turbulent modes have larger associated velocities than the clouds' internal velocity dispersions. Structural characterization algorithms have started to distinguish the best fitting simulations to a particular observation, and have opened several new questions, such as the nature of the observed line width-size relation and of the relation between the structures seen in channel maps and the true spatial distribution of the density and velocity fields. The velocity field apparently dominates the morphology seen in intensity channel maps, at least in cases when the density field exhibits power spectra steep enough. Furthermore, the selection of scattered fluid parcels along the line of sight (LOS) by their LOS-velocity inherent to the construction of spectroscopic data may introduce spurious small-scale structure in high spectral resolution channel maps.

TURBULENT FORMATION OF INTERSTELLAR STRUCTURES AND THE CONNECTION BETWEEN SIMULATIONS AND OBSERVATIONS