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dc.contributordli@arm.ac.uk; Armagh Observatory and Planetarium College Hill, Armagh, BT61 9DG, UK; School of Mathematics and Physics, Queen's University Belfast University Road, Belfast, BT7 1NN, UK; ;
dc.contributorArmagh Observatory and Planetarium College Hill, Armagh, BT61 9DG, UK
dc.contributor.authorLi, Daohai
dc.contributor.authorChristou, Apostolos A.
dc.date.accessioned2024-04-04T11:49:16Z
dc.date.available2024-04-04T11:49:16Z
dc.date.issued2017-11-01T00:00:00Z
dc.identifier.doi10.3847/1538-3881/aa8fc9
dc.identifier.other2017AJ....154..209L
dc.identifier.other10.3847/1538-3881/aa8fc9
dc.identifier.other0000-0002-8683-1758
dc.identifier.other-
dc.identifier.urihttp://hdl.handle.net/20.500.14302/2034
dc.description.abstractAmong the irregular satellites orbiting Jupiter, the Himalia family is characterized by a high velocity dispersion δ v of several hundred ms<SUP>-1</SUP> among its members, inconsistent with a collisional origin. Efforts to account for this through internecine gravitational interactions do not readily reproduce this feature. Here, we revisit the problem in the context of recent cosmogonical models, where the giant planets migrated significantly through interaction with a planetesimal disk and suffered encounters with planetesimals and planet-sized objects. Our starting assumption is that family formation either predated this phase or occurred soon after its onset. We simulate numerically the diffusive effect of three distinct populations of perturbers on a set of test particles representing the family: Moon-sized (MPT) and Pluto-sized (PPT) planetesimals, and planetary-mass objects (PMO) with masses typical of ice-giant planets. We find that PPT flybys are inefficient, but encounters with MPTs raise the δ v of ∼60% of our test particles to &gt; 200 ms<SUP>-1</SUP> with respect to Himalia, in agreement with observations. As MPTs may not have been abundant in the disk, we simulate encounters between Jupiter and PMOs. We find that too few encounters generate less dispersion than MPTs while too many essentially destroy the family. For PMO masses in the range 5-20 m<SUB>\oplus</SUB>, the family orbital distribution is reproduced by a few tens of encounters.
dc.publisherThe Astronomical Journal
dc.titleOrbital Modification of the Himalia Family during an Early Solar System Dynamical Instability
dc.typearticle
dc.source.journalAJ
dc.source.journalAJ....154
dc.source.volume154
refterms.dateFOA2024-04-04T11:49:16Z
dc.identifier.bibcode2017AJ....154..209L


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