2026ApJ...998..169H

Hydrodynamic simulations of planet-disk interactions often show material accumulation near the co-orbital Lagrange points L₄ and L₅-features that may correspond to observed crescents in protoplanetary disks. Intriguingly, these simulations also show an asymmetrical distribution of gas between L₄ and L₅, whose physical origin is not yet understood and could allow us to further constrain the inner workings of planet-disk interactions. We performed 2D hydrodynamic simulations of a single, nonmigrating planet embedded in a gaseous disk to investigate this effect. We find that the asymmetry is primarily controlled by the sign of the radial temperature gradient, with positive gradients enhancing the accumulation at L₄ and negative ones enhancing L₅. A symmetric distribution is recovered on globally isothermal disks. Furthermore, we find that the azimuthal locations of L₄ and L₅ deviate from the classical circular restricted three-body problem, following a monotonic trend with the disk pressure scale height h_p: ${\phi }_{\,\rm{max}\,}\approx \pm 60^\circ [1+0.18{({h}_{p}^{3}{M}_{\star }/{m}_{p})}^{2/3}]$. Our simulations show that the longest-lived and largest-amplitude structures are produced by planets opening gaps with depths Σ_gap/Σ₀ ≲ 0.2. We successfully reproduce the observed asymmetry using a semianalytical model that incorporates the azimuthally asymmetric radial velocity background induced by the planet. Overall, our results suggest that asymmetries in the form of crescents and clumps inside of density gaps opened by planets can constrain the local thermodynamic properties of protoplanetary disks.