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Multiple Stellar Encounters on Protoplanetary Disks in Birth Clusters of Stars

Jiménez-Torres J. J.

Acta Astronomica

2020

Vol. 70, No. 1

53--74

We investigate the orbital modification of planetesimals in protoplanetary disks due to multiple stellar encounters in star formation clusters. We modeled multiple encounters with different flyby masses ranging from 0.02 M⊙ up to 0.5 M⊙, approach distances within 400 a.u. and virial velocities to simulate conditions of encounters in star formation regions. We propose an analysis of mass densities as a function of time and found that densities from 3×103 M⊙/pc3 to 1.4×104 M⊙/pc3 can produce from one up to three stellar encounters on a cross sectional area with a radius of 400 a.u. containing a 100 a.u. planetary disk in a period of time of 1×106 yr. We found that the orbital structure of observed transneptunian objects such as 2005 QU182 and the sednoid 2012 VP113 can simultaneously be produced with multiple encounters. We also found that the effect of multiple encounters with low mass stars (<0.5 M⊙) can reproduce similar orbital eccentricities and inclinations as produced by a single stellar encounter with a mass in the order of 1 M⊙. This corresponds to a realistic scenario considering that low mass stars represent the majority of the new born stars in a birth cluster of stars. We provide a relation between the number of stellar encounters on a cross sectional area and the stellar mass density. With interferometers such as ALMA, the influence of stellar encounters in star formation regions may become testable, which suggests the incorporation of different planetary disk conditions in future studies.