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Dust rings in TW Hya

Ijtsma, Manou (2019) Dust rings in TW Hya. Research Project, Science Education and Communication.

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Abstract

Recent high spatial resolution ALMA observations show a ringed substructure in the protoplanetary disk of the nearby T Tauri star TW Hya. With the help of a thermo-chemical disk code called ProDiMo which calculates both, the continuum radiative transfer and the gas thermal balance/chemistry, the influence of this substructure on the gas will be investigated. The starting point for this thesis is an existing protoplanetary disk model from the DIANA project which has a smooth surface density and hence also surface brightness profile. Modifications of this model will be made to match the model as good as possible to the observed surface brightness profile. From the final run it could be concluded that the disk mass went down by 34 %. The substructure of the rings has caused the dust temperature in the outer regions of the disk to increase. The gas temperatures did not show a big deviation, but the CO iceline was shifted resulting in an increase of the CO ice mass of 8.5 *10^(-8) Msun. The smallest change in line fluxes between the original model and the DIANA model is Fline = 1.36 *10^(-21) W/m^2, which should be detectable by ALMA. The final model is also compared to an existing disk model of TW Hya by van Boekel et al., (2017) which matches the gas surface density within a factor two, but the surface density of the large grains with sizes 1-10 mm differs by a factor 30. The reason for this difference is not found as the Boekel et al., (2017) paper gives to little insight in the modeling method used to obtain this profile.

Item Type: Thesis (Research Project)
Supervisor:
Supervisor nameSupervisor E mail
Kamp, I.E.E.I.E.E.Kamp@rug.nl
Degree programme: Science Education and Communication
Thesis type: Research Project
Language: English
Date Deposited: 11 Mar 2019
Last Modified: 13 Mar 2019 08:50
URI: http://fse.studenttheses.ub.rug.nl/id/eprint/19253

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