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Please use this identifier to cite or link to this item: https://research.matf.bg.ac.rs/handle/123456789/2991
DC FieldValueLanguage
dc.contributor.authorVukotic, Branislav Men_US
dc.contributor.authorArbutina, Bojanen_US
dc.contributor.authorUrošević, Dejanen_US
dc.date.accessioned2025-12-12T15:15:36Z-
dc.date.available2025-12-12T15:15:36Z-
dc.date.issued2006-
dc.identifier.urihttps://research.matf.bg.ac.rs/handle/123456789/2991-
dc.description.abstractIn this paper we present a brief discussion of the magnetic field (H) evolution in supernova remnant (SNRs). Evolution models generally assume H ∝ D−δ . Knowing δ would be particularly important in the study of the radio surface brightness to diameter (Σ − D) relation for SNRs, since it would allow us to compare different theoretical models for the radio evolution.en_US
dc.language.isoenen_US
dc.publisherBeograd : Astronomska opservatorijaen_US
dc.relation.ispartofPublications of the Astronomical Observatory of Belgradeen_US
dc.titleModels of the magnetic field evolution in supernova remnantsen_US
dc.typeConference Objecten_US
dc.relation.conferenceNational Conference of Astronomers of Serbia and Montenegro (14 ; 2005 ; Beograd)en_US
dc.relation.publicationProceedings of the 14th National Conference of Astronomers of Serbia and Montenegroen_US
dc.identifier.urlhttps://publications.aob.rs/80/pdf/095-097.pdf-
dc.contributor.affiliationAstronomyen_US
dc.contributor.affiliationAstronomyen_US
dc.relation.isbn86-80019-07-0en_US
dc.relation.issn0373-3742en_US
dc.description.rankM63en_US
dc.relation.firstpage95en_US
dc.relation.lastpage97en_US
dc.relation.issue80en_US
item.openairetypeConference Object-
item.languageiso639-1en-
item.grantfulltextnone-
item.openairecristypehttp://purl.org/coar/resource_type/c_18cf-
item.fulltextNo Fulltext-
item.cerifentitytypePublications-
crisitem.author.deptAstronomy-
crisitem.author.deptAstronomy-
crisitem.author.orcid0000-0002-8036-4132-
crisitem.author.orcid0000-0003-0665-0939-
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