Observability of planet-disc interactions in CO kinematics
Author
dc.contributor.author
Pérez, Sebastián
Author
dc.contributor.author
Casassus Montero, Simón
Author
dc.contributor.author
Benítez-Llambay, P.
Admission date
dc.date.accessioned
2019-05-31T15:21:16Z
Available date
dc.date.available
2019-05-31T15:21:16Z
Publication date
dc.date.issued
2018
Cita de ítem
dc.identifier.citation
Monthly Notices of the Royal Astronomical Society: Letters, Volumen 480, Issue 1, 2018, Pages L12-L17.
Identifier
dc.identifier.issn
17453933
Identifier
dc.identifier.issn
17453925
Identifier
dc.identifier.other
10.1093/mnrasl/sly109
Identifier
dc.identifier.uri
https://repositorio.uchile.cl/handle/2250/169553
Abstract
dc.description.abstract
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 in CO rotational emission lines. We perform 3D hydrodynamical simulations of single giant planets and predict the emergent intensity field with radiative transfer. Pressure gradients at planet-carved gaps, spiral wakes, and vortices bear strong kinematic counterparts. The isovelocity contours in the CO(2-1) line centroids vo reveal large-scale perturbations, corresponding to abrupt transitions from below sub-Keplerian to super-Keplerian rotation along with radial and vertical flows. The increase in line optical depth at the edge of the gap also modulates vo, but this is a mild effect compared to the dynamical imprint of the planet-disc interaction. The large-scale deviations from the Keplerian rotation
thus allow the planets to be indirectly detected via the first moment maps of molecular gas
tracers, at Atacama Large Millimetre/submillimetre Array angular resolutions. The strength
of these deviations depends on the mass of the perturber. This initial study paves the way to
eventually determine the mass of the planet by comparison with more detailed models.