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Gap-opening planets can generate dust-trapping vortices that may explain someof the latest discoveries of high-contrast crescent-shaped dust asymmetries intransition discs. While planet-induced vortices were previously thought to haveconcentrated shapes, recent computational work has shown that these featuresnaturally become much more elongated in the gas when simulations account forthe relatively long timescale over which planets accrete their mass. In thiswork, we conduct two-fluid hydrodynamical simulations of vortices induced byslowly-growing Jupiter-mass planets in discs with very low viscosity ($\alpha =3 \times 10^{-5}$). We simulate the dust dynamics for four particle sizesspanning 0.3 mm to 1 cm in order to produce synthetic ALMA images. In oursimulations, we find that an elongated vortex still traps dust, but notdirectly at its center. With a flatter pressure bump and disruptions from theplanet's overlapping spiral density waves, the dust instead circulates aroundthe vortex. This motion (1) typically carries the peak off-center, (2) spreadsthe dust out over a wider azimuthal extent $\geq 180^{\circ}$, (3) skews theazimuthal profile towards the front of the vortex, and (4) can also createdouble peaks in newly-formed vortices. In particular, we expect that the mostdefining observational signature, a peak offset of more than $30^{\circ}$,should be detectable $>30\%$ of the time in observations with a beam diameterof at most the planet's separation from its star.

Observational diagnostics of elongated planet-induced vortices with realistic planet formation timescales