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dc.contributor.authorSiegert, Thomas
dc.contributor.authorPleintinger, Moritz M. M.
dc.contributor.authorDiehl, Roland
dc.contributor.authorKrause, Martin G. H.
dc.contributor.authorGreiner, Jochen
dc.contributor.authorWeinberger, Christoph
dc.date.accessioned2023-04-12T10:45:01Z
dc.date.available2023-04-12T10:45:01Z
dc.date.issued2023-03-30
dc.identifier.citationSiegert , T , Pleintinger , M M M , Diehl , R , Krause , M G H , Greiner , J & Weinberger , C 2023 , ' Galactic Population Synthesis of Radioactive Nucleosynthesis Ejecta ' , Astronomy & Astrophysics , vol. 672 . https://doi.org/10.1051/0004-6361/202244457
dc.identifier.issn0004-6361
dc.identifier.otherArXiv: http://arxiv.org/abs/2301.10192v1
dc.identifier.otherORCID: /0000-0002-9610-5629/work/133139511
dc.identifier.urihttp://hdl.handle.net/2299/26161
dc.description© The Authors 2023. This is an Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0).
dc.description.abstractDiffuse gamma-ray line emission traces freshly produced radioisotopes in the interstellar gas, providing a unique perspective on the entire Galactic cycle of matter from nucleosynthesis in massive stars to their ejection and mixing in the interstellar medium. We aim at constructing a model of nucleosynthesis ejecta on galactic scale which is specifically tailored to complement the physically most important and empirically accessible features of gamma-ray measurements in the MeV range, in particular for decay gamma-rays such as $^{26}$Al, $^{60}$Fe or $^{44}$Ti. Based on properties of massive star groups, we developed a Population Synthesis Code which can instantiate galaxy models quickly and based on many different parameter configurations, such as the star formation rate, density profiles, or stellar evolution models. As a result, we obtain model maps of nucleosynthesis ejecta in the Galaxy which incorporate the population synthesis calculations of individual massive star groups. Based on a variety of stellar evolution models, supernova explodabilities, and density distributions, we find that the measured $^{26}$Al distribution from INTEGRAL/SPI can be explained by a Galaxy-wide population synthesis model with a star formation rate of $4$-$8\,\mathrm{M_{\odot}\,yr^{-1}}$ and a spiral-arm dominated density profile with a scale height of at least 700 pc. Our model requires that most massive stars indeed undergo a supernova explosion. This corresponds to a supernova rate in the Milky Way of $1.8$-$2.8$ per century, with quasi-persistent $^{26}$Al and $^{60}$Fe masses of $1.2$-$2.4\,\mathrm{M_{\odot}}$ and $1$-$6\,\mathrm{M_{\odot}}$, respectively. Comparing the simulated morphologies to SPI data suggests that a frequent merging of superbubbles may take place in the Galaxy, and that an unknown but strong foreground emission at 1.8 MeV could be present.en
dc.format.extent19
dc.format.extent10136225
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysics
dc.subjectastro-ph.GA
dc.subjectastro-ph.HE
dc.titleGalactic Population Synthesis of Radioactive Nucleosynthesis Ejectaen
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Engineering & Computer Science
dc.contributor.institutionDepartment of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.versionofrecord10.1051/0004-6361/202244457
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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