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Please use this identifier to cite or link to this item: https://research.matf.bg.ac.rs/handle/123456789/831
DC FieldValueLanguage
dc.contributor.authorOpsenica, S.en_US
dc.contributor.authorArbutina, Bojanen_US
dc.date.accessioned2022-08-15T17:38:18Z-
dc.date.available2022-08-15T17:38:18Z-
dc.date.issued2011-01-01-
dc.identifier.issn1450698X-
dc.identifier.urihttps://research.matf.bg.ac.rs/handle/123456789/831-
dc.description.abstractWe present IDL (Interactive Data Language) codes for fitting a theoretical emission profile of a shell supernova remnant (SNR) to the mean profile of an SNR obtained from radio observations. Two considered theoretical models are: 1) a shell with constant emissivity and 2) a synchrotron shell with radially aligned magnetic field. The codes were applied to several observed supernova remnants. Good results are obtained in five considered cases, which justify the use of our code for remnants that are bright (so that observational errors are not large) and spherically symmetric enough.en_US
dc.relation.ispartofSerbian Astronomical Journalen_US
dc.subjectG127.1+0.5en_US
dc.subjectG132.7+1.3en_US
dc.subjectG332.0+0.2en_US
dc.subjectG54.4-0.3en_US
dc.subjectISM: individual objects: G17.8-2.6en_US
dc.subjectISM: supernova remnantsen_US
dc.subjectMethods: numericalen_US
dc.subjectRadio continuum: ISMen_US
dc.titleNumerical code for fitting radial emission profile of a shell supernova remnant. Applicationen_US
dc.typeArticleen_US
dc.identifier.doi10.2298/SAJ1183077O-
dc.identifier.scopus2-s2.0-84884229375-
dc.identifier.urlhttps://api.elsevier.com/content/abstract/scopus_id/84884229375-
dc.contributor.affiliationAstronomyen_US
dc.relation.firstpage77en_US
dc.relation.lastpage85en_US
dc.relation.issue183en_US
item.fulltextNo Fulltext-
item.openairetypeArticle-
item.grantfulltextnone-
item.openairecristypehttp://purl.org/coar/resource_type/c_18cf-
item.cerifentitytypePublications-
crisitem.author.deptAstronomy-
crisitem.author.orcid0000-0002-8036-4132-
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