Observability of planet–disc interactions in CO kinematics

• DOI: 10.1093/mnrasl/sly109
• Publication Date: 2018-06-15T11:07:54Z
• Authors: Sebastián Pérez; S Casassus; P Benítez-Llambay
• Keywords: Giant planet; Line (geometry)

Empirical evidence of planets in gas-rich circumstellar discs is required to constrain giant planet formation theories. Here we study the kinematic patterns which arise from planet-disc interactions and their observability CO rotational emission lines. We perform three-dimensional hydrodynamical simulations single planets, predict emergent intensity field with radiative transfer. Pressure gradients at planet-carved gaps, spiral wakes vortices bear strong counterparts. The iso-velocity contours CO(2-1) line centroids $v_\circ$ reveal large-scale perturbations, corresponding abrupt transitions below sub-Keplerian super-Keplerian rotation along radial vertical flows. increase optical depth edge gap also modulates $v_\circ$, but this a mild effect compared dynamical imprint interaction. deviations Keplerian thus allow be indirectly detected via first moment maps molecular gas tracers, ALMA angular resolutions. strength these depends on mass perturber. This initial paves way eventually determine by comparison more detailed models.