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Fig. 5

image

Pressure gradient in different gas accretion models for m = 0.5 MJ. Even though the different models present different inner disc structures at the same planetary mass, the difference in the pressuregradients is too small to be observationally resolved. The bump located at the planet position is due to the material around the planet location. It vanishes with higher accretion rates as the planet accretes all the material at this location.

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