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

Spatially resolved continuum observations of planet-forming disks showprominent ring and gap structures in their dust distribution. However, thepicture from gas observations is much less clear and constraints on the radialgas density structure (i.e. gas gaps) remain rare and uncertain. We want toinvestigate the importance of thermo-chemical processes for the interpretationof high-spatial-resolution gas observations of planet-forming disks and theirimpact on derived gas properties. We apply the radiation thermo-chemical diskcode ProDiMo (PROtoplanetary DIsk MOdel) to model self-consistently the dustand gas disk of HD 163296, using the DSHARP gas and dust observations. Withthis model we investigate the impact of dust gaps and gas gaps, consideringchemistry and heating/cooling processes, on the observables and the derived gasproperties. We find distinct peaks in the radial line intensity profiles of theCO line data of HD 163296 at the location of the dust gaps. Our model indicatesthat those peaks are not only a consequence of a gas temperature increasewithin the gaps but are mainly caused by the absorption of line emission fromthe back side of the disk by the dust rings. For two of the three prominentdust gaps in HD 163296, we find that thermo-chemical effects are negligible forderiving density gradients via measurements of the rotation velocity. However,for the gap with the highest dust depletion, the temperature gradient can bedominant and needs to be considered to derive accurate gas density profiles.Self-consistent gas and dust thermo-chemical modelling in combination withhigh-quality observations of multiple molecules are necessary to accuratelyderive gas gap depths and shapes. This is crucial to determine the origin ofgaps and rings in planet-forming disks and to improve the mass estimates offorming planets if they are the cause of the gap.

Interpreting high spatial resolution line observations of planet-forming disks with gaps and rings -- The case of HD 163296