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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We derive the spectral energy distribution (SED) of dusty, isothermal, selfgravitating, stable and spherical clouds externally heated by the ambientinterstellar radiation field. For a given radiation field and dust properties,the radiative transfer problem is determined by the pressure of the surroundingmedium and the cloud mass expressed as a fraction of the maximum stable cloudmass above which the clouds become gravitational unstable.  To solve the radiative transfer problem a ray-tracing code is used toaccurately derive the light distribution inside the cloud. This code considersboth non isotropic scattering on dust grains and multiple scattering events.The dust properties inside the clouds are assumed to be the same as in thediffuse interstellar medium in our galaxy. We analyse the effect of thepressure, the critical mass fraction, and the ISRF on the SED and presentbrightness profiles in the visible, the IR/FIR and the submm/mm regime with thefocus on the scattered emission and the thermal emission from PAH-molecules anddust grains.

The Spectral Energy Distribution of Self-gravitating Interstellar Clouds I. Spheres