Deutsch
 
Hilfe Datenschutzhinweis Impressum
  DetailsucheBrowse

Datensatz

DATENSATZ AKTIONENEXPORT

Freigegeben

Konferenzband

The gas structure of the HD 163296 planet-forming disk - gas gaps or not?

MPG-Autoren
/persons/resource/persons172897

Thi,  W.-F.
Center for Astrochemical Studies at MPE, MPI for Extraterrestrial Physics, Max Planck Society;

Externe Ressourcen
Es sind keine externen Ressourcen hinterlegt
Volltexte (beschränkter Zugriff)
Für Ihren IP-Bereich sind aktuell keine Volltexte freigegeben.
Volltexte (frei zugänglich)
Es sind keine frei zugänglichen Volltexte in PuRe verfügbar
Ergänzendes Material (frei zugänglich)
Es sind keine frei zugänglichen Ergänzenden Materialien verfügbar
Zitation

Rab, C., Muro-Arena, G. A., Kamp, I., Dominik, C., Waters, L. B. F. M., Thi, W.-F., et al. (2020). The gas structure of the HD 163296 planet-forming disk - gas gaps or not?. Cambridge, UK: Cambridge University Press.


Zitierlink: https://hdl.handle.net/21.11116/0000-0008-15E3-0
Zusammenfassung
HD 163296 is a young star surrounded by a planet-forming disk that shows clear signatures of dust gaps and rings; likely an indication of ongoing planet formation. We use the radiation thermochemical disk code ProDiMo to investigate the impact of dust/gas gaps on the temperature, chemistry and observables. Furthermore, we model high spatial resolution gas and dust observation of HD 163296 (ALMA/DSHARP). Our first results indicate that features in the observed radial intensity profile of the 12CO line are a consequence of the dust gaps and do not require gas depletion. Those preliminary results indicate that self-consistent modelling of the gas (chemistry, heating/cooling) and dust is necessary to accurately infer the degree of gas depletion within dust gaps. Such information is crucial to understand the processes that generate the disk substructure and their relation to planet formation.