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@ARTICLE{Pfalzner:904521,
      author       = {Pfalzner, Susanne and Govind, Amith},
      title        = {{C}lose {S}tellar {F}lybys {C}ommon in {L}ow-mass
                      {C}lusters},
      journal      = {The astrophysical journal / 1},
      volume       = {921},
      number       = {1},
      issn         = {0004-637X},
      address      = {London},
      publisher    = {Institute of Physics Publ.},
      reportid     = {FZJ-2021-06091},
      pages        = {90 -},
      year         = {2021},
      abstract     = {Numerous protoplanetary disks show distinct spiral arms
                      features. While possibly caused by a range of processes,
                      detailed pattern analysis points at close stellar flybys as
                      cause for some of them. Surprisingly, these disks reside in
                      young low-mass clusters, where close stellar flybys are
                      expected to be rare. This fact motivated us to take a fresh
                      look at the frequency of close flybys in low-mass clusters.
                      In the solar neighborhood, low-mass clusters have smaller
                      half-mass radii than their more massive counterparts. We
                      show that this observational fact results in the mean and
                      central stellar density of low-mass clusters being
                      approximately the same as in high-mass clusters, which is
                      rarely reflected in theoretical studies. We perform N-body
                      simulations of the stellar dynamics in young clusters
                      obeying the observed mass–radius relation. Taking the mean
                      disk truncation radius as a proxy for the degree of
                      influence of the environment, we find that the influence of
                      the environment on disks is more or less the same in low-
                      and high-mass clusters. Even the fraction of small disks
                      (<10 au) is nearly identical. Our main conclusion is that
                      the frequency of close flybys seems to have been severely
                      underestimated for low-mass clusters. A testable prediction
                      of this hypothesis is that low-mass clusters should contain
                      $10\%–15\%$ of disks smaller than 30 au truncated by
                      flybys. These truncated disks should be distinguishable from
                      primordially small disks by their steep outer edge.},
      cin          = {JSC},
      ddc          = {520},
      cid          = {I:(DE-Juel1)JSC-20090406},
      pnm          = {5111 - Domain-Specific Simulation $\&$ Data Life Cycle Labs
                      (SDLs) and Research Groups (POF4-511)},
      pid          = {G:(DE-HGF)POF4-5111},
      typ          = {PUB:(DE-HGF)16},
      UT           = {WOS:000716744900001},
      doi          = {10.3847/1538-4357/ac19aa},
      url          = {https://juser.fz-juelich.de/record/904521},
}