Dust trapping around Lagrangian points in protoplanetary disks

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dc.contributor.authorMontesinos, Matias
dc.contributor.authorGarrido-Deutelmoser, Juan
dc.contributor.authorOlofsson, Johan
dc.contributor.authorGiuppone, Cristian A.
dc.contributor.authorCuadra, Jorge
dc.contributor.authorBayo, Amelia
dc.contributor.authorSucerquia, Mario
dc.contributor.authorCuello, Nicolas
dc.date.accessioned2025-01-23T19:47:19Z
dc.date.available2025-01-23T19:47:19Z
dc.date.issued2020
dc.description.abstractAims. Trojans are defined as objects that share the orbit of a planet at the stable Lagrangian points L-4 and L-5. In the Solar System, these bodies show a broad size distribution ranging from micrometer (mu m) to centimeter (cm) particles (Trojan dust) and up to kilometer (km) rocks (Trojan asteroids). It has also been theorized that earth-like Trojans may be formed in extra-solar systems. The Trojan formation mechanism is still under debate, especially theories involving the effects of dissipative forces from a viscous gaseous environment.
dc.description.abstractMethods. We perform hydro-simulations to follow the evolution of a protoplanetary disk with an embedded 1-10 Jupiter-mass planet. On top of the gaseous disk, we set a distribution of mu m-cm dust particles interacting with the gas. This allows us to follow dust dynamics as solids get trapped around the Lagrangian points of the planet.
dc.description.abstractResults. We show that large vortices generated at the Lagrangian points are responsible for dust accumulation, where the leading Lagrangian point L-4 traps a larger amount of submillimeter (submm) particles than the trailing L-5, which traps mostly mm-cm particles. However, the total bulk mass, with typical values of similar to M-moon, is more significant in L-5 than in L-4, in contrast to what is observed in the current Solar System a few gigayears later. Furthermore, the migration of the planet does not seem to affect the reported asymmetry between L-4 and L-5.
dc.description.abstractConclusions. The main initial mass reservoir for Trojan dust lies in the same co-orbital path of the planet, while dust migrating from the outer region (due to drag) contributes very little to its final mass, imposing strong mass constraints for the in situ formation scenario of Trojan planets.
dc.fuente.origenWOS
dc.identifier.doi10.1051/0004-6361/202038758
dc.identifier.eissn1432-0746
dc.identifier.issn0004-6361
dc.identifier.urihttps://doi.org/10.1051/0004-6361/202038758
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/100371
dc.identifier.wosidWOS:000586586300004
dc.language.isoen
dc.revistaAstronomy & astrophysics
dc.rightsacceso restringido
dc.subjectplanets and satellites: formation
dc.subjectplanet-disk interactions
dc.subjectprotoplanetary disks
dc.titleDust trapping around Lagrangian points in protoplanetary disks
dc.typeartículo
dc.volumen642
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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