The DACs and SACs effects from stars to Quasars. Some first general notices

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The DACs and SACs effects from stars to Quasars. Some first general notices

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dc.contributor.author Danezis, E.
dc.contributor.editor Popović, Luka Č.
dc.date.accessioned 2011-01-10T10:39:13Z
dc.date.available 2011-01-10T10:39:13Z
dc.date.issued 2007
dc.identifier.isbn 978-86-80019-17-8 en_US
dc.identifier.uri http://hdl.handle.net/123456789/1453
dc.description.provenance Submitted by Slavisha Milisavljevic (slavisha) on 2011-01-10T10:39:13Z No. of bitstreams: 1 I05.pdf: 2063970 bytes, checksum: 7700134e20a70de0c807cb2f1c727230 (MD5) en
dc.description.provenance Made available in DSpace on 2011-01-10T10:39:13Z (GMT). No. of bitstreams: 1 I05.pdf: 2063970 bytes, checksum: 7700134e20a70de0c807cb2f1c727230 (MD5) Previous issue date: 2007 en
dc.language.iso en en_US
dc.publisher Nenad Milovanović & Milan S. Dimitrijević, Astronomical Observatory, Belgrade en_US
dc.title The DACs and SACs effects from stars to Quasars. Some first general notices en_US
mf.subject.keywords The spectra of Hot Emission Stars and AGN present peculiar profiles that result from dynamical processes such as accretion and/or ejection of matter from these objects. In this paper we explain the idea of DACs and SACs phenomena, as a reason of spectral lines peculiarity in Hot Emission Stars and AGN. We present the line function of a kinematical model enabling us to study the physical parameters of the density regions in the plasma surrounding of the studied objects, where DACs and SACs of a spectral line are created, producing the observed peculiar profiles. Using this model, we study some AGN spectral lines and we present an analysis of the physical parameters of the regions that these spectral lines arise from. We also present some first general conclusions, derived from the proposed model, including the relations among the physical parameters of the density regions of the plasma surrounding the Oe stars, where DACs and SACs are created, producing the observed peculiar profiles. Finally we present a first comparison of DACs and SACs phenomena between Be and Oe stars. en_US
mf.document.pages 85 en_US
mf.contributor.editor-in-chief Dimitrijević, S. Milan

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