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@ARTICLE{Pfalzner:862175,
      author       = {Pfalzner, Susanne and Bannister, Michele T.},
      title        = {{A} {H}ypothesis for the {R}apid {F}ormation of {P}lanets},
      journal      = {The astrophysical journal / 2 Letters Part 2},
      volume       = {874},
      number       = {2},
      issn         = {2041-8213},
      address      = {London},
      publisher    = {Institute of Physics Publ.},
      reportid     = {FZJ-2019-02523},
      pages        = {L34 -},
      year         = {2019},
      abstract     = {The discovery of 1I/'Oumuamua confirmed that planetesimals
                      must exist in great numbers in interstellar space.
                      Originally generated during planet formation, they are
                      scattered from their original systems and subsequently drift
                      through interstellar space. As a consequence they should
                      seed molecular clouds with at least hundred-meter-scale
                      objects. We consider how the galactic background density of
                      planetesimals, enriched from successive generations of star
                      and system formation, can be incorporated into forming
                      stellar systems. We find that at a minimum of the order of
                      107 'Oumuamua-sized and larger objects, plausibly including
                      hundred-kilometer-scale objects, should be present in
                      protoplanetary disks. At such initial sizes, the growth
                      process of these seed planetesimals in the initial gas- and
                      dust-rich protoplanetary disks is likely to be substantially
                      accelerated. This could resolve the tension between
                      accretionary timescales and the observed youth of fully
                      fledged planetary systems. Our results strongly advocate
                      that the population of interstellar planetesimals should be
                      taken into account in future studies of planet formation. As
                      not only the Galaxy's stellar metallicity increased over
                      time but also the density of interstellar objects, we
                      hypothesize that this enriched seeding accelerates and
                      enhances planetary formation after the first couple of
                      generations of planetary systems.},
      cin          = {JSC},
      ddc          = {520},
      cid          = {I:(DE-Juel1)JSC-20090406},
      pnm          = {511 - Computational Science and Mathematical Methods
                      (POF3-511)},
      pid          = {G:(DE-HGF)POF3-511},
      typ          = {PUB:(DE-HGF)16},
      UT           = {WOS:000518383700007},
      doi          = {10.3847/2041-8213/ab0fa0},
      url          = {https://juser.fz-juelich.de/record/862175},
}