Observations have shown indirect evidence of a population of massive planets embedded in protoplanetary disks, whose interactions with the disk would substantially impact its structure.

We studied how a fairly massive forming planet would affect the 3D gas velocity structure of a VSI-turbulent planet-forming disk,  focused on the observability of kinematical signatures (paper accepted to A&A).

The vertical shear instability (VSI) is an hydrodynamical instability, candidate to generate turbulence in protoplanetary disks.

In Barraza et al. 2021, we studied the feasibility of observing large-scale motions produced by the VSI in deep high-resolution ALMA CO kinematic observations. 

We found that ALMA has the capability to detect the corrugated velocity structure generated by VSI, potentially revealing it as a source of turbulence in disks outer regions. 

Large-scale spiral arms structures have been observed in multi-wavelength protoplanetary disks, yet their nature is still a puzzle. In Brown-Sevilla et al. 2021, I contributed with 2D hydrodynamical simulations exploring the scenario in which the spirals observed in WaOph 6 are triggered by a massive planet. 

In order to create the observed spiral structure, a putative 10 Jupiter-mass planet located on the outskirts of the disk is needed. However, this scenario is in tension with current companion mass upper limits and mm-dust trapping theories.