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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/8269
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dc.contributor.authorVasiliev, Evgenii O.-
dc.contributor.authorShchekinov, Yuri A.-
dc.date.accessioned2024-06-06T11:03:22Z-
dc.date.available2024-06-06T11:03:22Z-
dc.date.issued2023-12-09-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2023, Vol.527, p8755-8767en_US
dc.identifier.urihttp://hdl.handle.net/2289/8269-
dc.descriptionOpen Accessen_US
dc.description.abstractSupernovae (SNe) explosions are thought to be an important source of dust in galaxies. At the same time strong shocks from SNe are known as an efficient mechanism of dust destruction via thermal and kinetic sputtering. A critically important question of how these two hypotheses of SNe activity control the dust budget in galaxies is still not quite clearly understood. In this paper, we address this question within 3D multifluid hydrodynamical simulations, treating separately the SNe injected dust and the dust pre-existed in ambient interstellar gas. We focus primarily on how the injected and the pre-existing dust is destroyed by shock waves and hot gas in the SN bubble depending on the density of ambient gas. Within our model, we estimate an upper limit of the SN produced dust mass which can be supplied into interstellar medium. For an SN progenitor mass of 30 M and the ejected dust mass M d = 1 M , we constrain the dust mass that can be delivered into the ISM as ≥0.13 M , provided that the SN has injected large dust particles with a ≥0.1 μm.en_US
dc.language.isoenen_US
dc.publisherOxford University Press on behalf of Royal Astronomical Societyen_US
dc.relation.urihttps://ui.adsabs.harvard.edu/abs/2024MNRAS.527.8755V/abstracten_US
dc.relation.urihttps://arxiv.org/abs/2308.03106en_US
dc.relation.urihttps://doi.org/10.1093/mnras/stad3820en_US
dc.rights2023, The Author(s)en_US
dc.subjectdusten_US
dc.subjectextinction –ISMen_US
dc.subjectsupernova remnantsen_US
dc.titleDust evolution in a superno v a interacting with the ISMen_US
dc.typeArticleen_US
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