000364985 001__ 364985
000364985 005__ 20260216083657.0
000364985 0247_ $$2doi$$a10.1093/mnras/staf1577
000364985 0247_ $$2ISSN$$a0035-8711
000364985 0247_ $$2ISSN$$a1365-2966
000364985 0247_ $$2ISSN$$a1365-8711
000364985 0247_ $$2datacite_doi$$a10.15120/GSI-2026-00338
000364985 0247_ $$2WOS$$aWOS:001591043600001
000364985 037__ $$aGSI-2026-00338
000364985 082__ $$a520
000364985 1001_ $$00000-0003-1626-1355$$aRicigliano, Giacomo$$b0$$eCorresponding author
000364985 245__ $$aModelling the emission lines from r-process elements in supernova nebulae
000364985 260__ $$aOxford$$bOxford Univ. Press$$c2025
000364985 3367_ $$2DRIVER$$aarticle
000364985 3367_ $$2DataCite$$aOutput Types/Journal article
000364985 3367_ $$0PUB:(DE-HGF)16$$2PUB:(DE-HGF)$$aJournal Article$$bjournal$$mjournal$$s1769083840_3708053
000364985 3367_ $$2BibTeX$$aARTICLE
000364985 3367_ $$2ORCID$$aJOURNAL_ARTICLE
000364985 3367_ $$00$$2EndNote$$aJournal Article
000364985 500__ $$aThis is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/)
000364985 520__ $$aThe origin of heavy r-process elements in the Universe is still a matter   of great debate, with a confirmed scenario being neutron star (NS)   mergers. Additional relevant sites could be specific classes of events,   such as gamma-ray burst (GRB) supernova, short-plural form = SNe,   long-plural form = supernovae (SNs), where a central engine could push   neutron-rich material outwards, contributing to the ejecta of the   massive exploding star. Here, we investigate our ability to infer the   production of heavy elements in such scenarios, on the basis of the   observed nebular emission. We solve the steady-state ionization, level   population, and thermal balance, for optically thin ejecta in non-local   thermodynamic equilibrium (NLTE), in order to explore the role of heavy   elements in cooling the gas, and their imprint in the emergent spectrum   a few hundreds days post-explosion. We find that heavy elements would be   relevant in the cooling process of the nebula only if they account for   at least similar to 1 per cent of the total ejected mass, at the typical   kinetic temperatures of a few thousands K. However, even in the absence   of such amount, a few 0 . 1 per cent of the total ejected mass could be   instead sufficient to leave a detectable imprint around similar to 1-10   mu m . This wavelength range, which would be relatively clean from   features due to light elements, would be instead robustly populated by   lines from heavy elements arising from forbidden transitions in their   atomic fine structures. Hence, the new generation of telescopes,   represented by the James Webb Space Telescope (JWST), will most likely   allow for their detection.
000364985 536__ $$0G:(DE-HGF)POF4-612$$a612 - Cosmic Matter in the Laboratory (POF4-612)$$cPOF4-612$$fPOF IV$$x0
000364985 536__ $$0G:(GEPRIS)279384907$$aDFG project 279384907 - SFB 1245: Atomkerne: Von fundamentalen Wechselwirkungen zu Struktur und Sternen (279384907)$$c279384907$$x1
000364985 536__ $$0G:(DE-Ds200)ElementsHessen$$aElementsHessen - ELEMENTS : Exploring the Universe from microscopic to macroscopic scales (ELEMENTS cluster project) (ElementsHessen)$$cElementsHessen$$x2
000364985 588__ $$aDataset connected to CrossRef, Journals: repository.gsi.de
000364985 693__ $$0EXP:(DE-Ds200)no_experiment-20200803$$1EXP:(DE-Ds200)theory-20200803$$5EXP:(DE-Ds200)no_experiment-20200803$$atheory$$eno experiment theory work (theory)$$x0
000364985 7001_ $$aHotokezaka, Kenta$$b1
000364985 7001_ $$0P:(DE-Ds200)OR2242$$aArcones Segovia, Almudena$$b2
000364985 773__ $$0PERI:(DE-600)2016084-7$$a10.1093/mnras/staf1577$$gVol. 543, no. 3, p. 2534 - 2552$$n3$$p2534 - 2552$$tMonthly notices of the Royal Astronomical Society$$v543$$x0035-8711$$y2025
000364985 8564_ $$uhttps://repository.gsi.de/record/364985/files/staf1577.pdf$$yOpenAccess
000364985 8564_ $$uhttps://repository.gsi.de/record/364985/files/staf1577.pdf?subformat=pdfa$$xpdfa$$yOpenAccess
000364985 909CO $$ooai:repository.gsi.de:364985$$pdnbdelivery$$pdriver$$pVDB$$popen_access$$popenaire
000364985 9101_ $$0I:(DE-Ds200)20121206GSI$$6P:(DE-Ds200)OR2242$$aGSI Helmholtzzentrum für Schwerionenforschung GmbH$$b2$$kGSI
000364985 9131_ $$0G:(DE-HGF)POF4-612$$1G:(DE-HGF)POF4-610$$2G:(DE-HGF)POF4-600$$3G:(DE-HGF)POF4$$4G:(DE-HGF)POF$$aDE-HGF$$bForschungsbereich Materie$$lMatter and the Universe$$vCosmic Matter in the Laboratory$$x0
000364985 9141_ $$y2025
000364985 915__ $$0StatID:(DE-HGF)0200$$2StatID$$aDBCoverage$$bSCOPUS$$d2024-12-16
000364985 915__ $$0StatID:(DE-HGF)0160$$2StatID$$aDBCoverage$$bEssential Science Indicators$$d2024-12-16
000364985 915__ $$0LIC:(DE-HGF)CCBY4$$2HGFVOC$$aCreative Commons Attribution CC BY 4.0
000364985 915__ $$0StatID:(DE-HGF)0600$$2StatID$$aDBCoverage$$bEbsco Academic Search$$d2024-12-16
000364985 915__ $$0StatID:(DE-HGF)1150$$2StatID$$aDBCoverage$$bCurrent Contents - Physical, Chemical and Earth Sciences$$d2024-12-16
000364985 915__ $$0StatID:(DE-HGF)0501$$2StatID$$aDBCoverage$$bDOAJ Seal$$d2024-07-11T08:19:11Z
000364985 915__ $$0StatID:(DE-HGF)0500$$2StatID$$aDBCoverage$$bDOAJ$$d2024-07-11T08:19:11Z
000364985 915__ $$0StatID:(DE-HGF)0113$$2StatID$$aWoS$$bScience Citation Index Expanded$$d2024-12-16
000364985 915__ $$0StatID:(DE-HGF)0700$$2StatID$$aFees$$d2024-12-16
000364985 915__ $$0StatID:(DE-HGF)0150$$2StatID$$aDBCoverage$$bWeb of Science Core Collection$$d2024-12-16
000364985 915__ $$0StatID:(DE-HGF)9900$$2StatID$$aIF < 5$$d2024-12-16
000364985 915__ $$0StatID:(DE-HGF)0510$$2StatID$$aOpenAccess
000364985 915__ $$0StatID:(DE-HGF)0030$$2StatID$$aPeer Review$$bASC$$d2024-12-16
000364985 915__ $$0StatID:(DE-HGF)0561$$2StatID$$aArticle Processing Charges$$d2024-12-16
000364985 915__ $$0StatID:(DE-HGF)0100$$2StatID$$aJCR$$bMON NOT R ASTRON SOC : 2022$$d2024-12-16
000364985 915__ $$0StatID:(DE-HGF)0300$$2StatID$$aDBCoverage$$bMedline$$d2024-12-16
000364985 915__ $$0StatID:(DE-HGF)0420$$2StatID$$aNationallizenz$$d2024-12-16$$wger
000364985 915__ $$0StatID:(DE-HGF)0199$$2StatID$$aDBCoverage$$bClarivate Analytics Master Journal List$$d2024-12-16
000364985 9201_ $$0I:(DE-Ds200)KNA-20160901OR396$$kKNA$$lNukleare Astrophysik & Struktur$$x0
000364985 980__ $$ajournal
000364985 980__ $$aVDB
000364985 980__ $$aUNRESTRICTED
000364985 980__ $$aI:(DE-Ds200)KNA-20160901OR396
000364985 9801_ $$aFullTexts