Redistribution of CO at the location of the CO ice line in evolving gas and dust disks

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dc.contributor.authorMarkus Stammler, Sebastian
dc.contributor.authorBirnstiel, Tilman
dc.contributor.authorPanic, Olja
dc.contributor.authorDullemond, Cornelis Petrus
dc.contributor.authorDominik, Carsten
dc.date.accessioned2024-01-10T13:17:07Z
dc.date.available2024-01-10T13:17:07Z
dc.date.issued2017
dc.description.abstractContext. Ice lines are suggested to play a significant role in grain growth and planetesimal formation in protoplanetary disks. Evaporation fronts directly influence the gas and ice abundances of volatile species in the disk and therefore the coagulation physics and efficiency and the chemical composition of the resulting planetesimals. Aims. In this work, we investigate the influence of the existence of the CO ice line on particle growth and on the distribution of CO in the disk.
dc.description.abstractMethods. We include the possibility of tracking the CO content and/or other volatiles in particles and in the gas in our existing dust coagulation and disk evolution model and present a method for studying evaporation and condensation of CO using the Hertz-Knudsen equation. Our model does not yet include fragmentation, which will be part of further investigations.
dc.description.abstractResults. We find no enhanced grain growth immediately outside the ice line where the particle size is limited by radial drift. Instead, we find a depletion of solid material inside the ice line, which is solely due to evaporation of the CO. Such a depression inside the ice line may be observable and may help to quantify the processes described in this work. Furthermore, we find that the viscosity and diffusivity of the gas heavily influence the re-distribution of vaporized CO at the ice line and can lead to an increase in the CO abundance by up to a factor of a few in the region just inside the ice line. Depending on the strength of the gaseous transport mechanisms, the position of the ice line in our model can change by up to similar to 10AU and consequently, the temperature at that location can range from 21 to 23 K.
dc.description.funderDeutsche Forschungsgemeinschaft Schwerpunktprogramm
dc.description.funderPUC-HD Graduate Student Exchange Fellowship
dc.description.funderGerman Academic Exchange Service (DAAD)
dc.description.funderEuropean Union
dc.description.funderRoyal Society Dorothy Hodgkin Fellowship
dc.fechaingreso.objetodigital2024-05-07
dc.format.extent16 páginas
dc.fuente.origenWOS
dc.identifier.doi10.1051/0004-6361/201629041
dc.identifier.issn1432-0746
dc.identifier.urihttps://doi.org/10.1051/0004-6361/201629041
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/78638
dc.identifier.wosidWOS:000400754000035
dc.information.autorucAstrofísica;Stammler S;S/I;1055276
dc.language.isoen
dc.nota.accesocontenido parcial
dc.publisherEDP SCIENCES S A
dc.revistaASTRONOMY & ASTROPHYSICS
dc.rightsacceso restringido
dc.subjectprotoplanetary disks
dc.subjectaccretion,accretion disks
dc.subjectdiffusion
dc.subjectmethods: numerical
dc.subjectPROTOPLANETARY DISKS
dc.subjectPLANETESIMAL FORMATION
dc.subjectINTERSTELLAR GRAINS
dc.subjectCOLLISIONAL GROWTH
dc.subjectSOLAR NEBULA
dc.subjectCOAGULATION
dc.subjectEVOLUTION
dc.subjectINSTABILITIES
dc.subjectDIFFUSION
dc.subjectBREAKING
dc.titleRedistribution of CO at the location of the CO ice line in evolving gas and dust disks
dc.typeartículo
dc.volumen600
sipa.codpersvinculados1055276
sipa.indexWOS
sipa.indexScopus
sipa.trazabilidadCarga SIPA;09-01-2024
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