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@ARTICLE{Ricigliano:364985,
      author       = {Ricigliano, Giacomo and Hotokezaka, Kenta and Arcones
                      Segovia, Almudena},
      title        = {{M}odelling the emission lines from r-process elements in
                      supernova nebulae},
      journal      = {Monthly notices of the Royal Astronomical Society},
      volume       = {543},
      number       = {3},
      issn         = {0035-8711},
      address      = {Oxford},
      publisher    = {Oxford Univ. Press},
      reportid     = {GSI-2026-00338},
      pages        = {2534 - 2552},
      year         = {2025},
      note         = {This is an Open Access article distributed under the terms
                      of the Creative Commons Attribution License
                      (https://creativecommons.org/licenses/by/4.0/)},
      abstract     = {The origin of heavy r-process elements in the Universe is
                      still a matter of great debate, with a confirmed scenario
                      being neutron star (NS) mergers. Additional relevant sites
                      could be specific classes of events, such as gamma-ray burst
                      (GRB) supernova, short-plural form = SNe, long-plural form =
                      supernovae (SNs), where a central engine could push
                      neutron-rich material outwards, contributing to the ejecta
                      of the massive exploding star. Here, we investigate our
                      ability to infer the production of heavy elements in such
                      scenarios, on the basis of the observed nebular emission. We
                      solve the steady-state ionization, level population, and
                      thermal balance, for optically thin ejecta in non-local
                      thermodynamic equilibrium (NLTE), in order to explore the
                      role of heavy elements in cooling the gas, and their imprint
                      in the emergent spectrum a few hundreds days post-explosion.
                      We find that heavy elements would be relevant in the cooling
                      process of the nebula only if they account for at least
                      similar to 1 per cent of the total ejected mass, at the
                      typical kinetic temperatures of a few thousands K. However,
                      even in the absence of such amount, a few 0 . 1 per cent of
                      the total ejected mass could be instead sufficient to leave
                      a detectable imprint around similar to 1-10 mu m . This
                      wavelength range, which would be relatively clean from
                      features due to light elements, would be instead robustly
                      populated by lines from heavy elements arising from
                      forbidden transitions in their atomic fine structures.
                      Hence, the new generation of telescopes, represented by the
                      James Webb Space Telescope (JWST), will most likely allow
                      for their detection.},
      cin          = {KNA},
      ddc          = {520},
      cid          = {I:(DE-Ds200)KNA-20160901OR396},
      pnm          = {612 - Cosmic Matter in the Laboratory (POF4-612) / DFG
                      project 279384907 - SFB 1245: Atomkerne: Von fundamentalen
                      Wechselwirkungen zu Struktur und Sternen (279384907) /
                      ElementsHessen - ELEMENTS : Exploring the Universe from
                      microscopic to macroscopic scales (ELEMENTS cluster project)
                      (ElementsHessen)},
      pid          = {G:(DE-HGF)POF4-612 / G:(GEPRIS)279384907 /
                      G:(DE-Ds200)ElementsHessen},
      experiment   = {$EXP:(DE-Ds200)no_experiment-20200803$},
      typ          = {PUB:(DE-HGF)16},
      UT           = {WOS:001591043600001},
      doi          = {10.1093/mnras/staf1577},
      url          = {https://repository.gsi.de/record/364985},
}