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dc.date.accessioned 2010-09-27T15:25:56Z
dc.date.available 2010-09-27T03:00:00Z
dc.date.issued 2001
dc.identifier.uri http://hdl.handle.net/10915/2084
dc.description.abstract The definition of Be stars (Jaschek et al. 1981) as non-supergiant B stars which at least once have shown some emission in the Balmer lines implies a vast phenomenology whose characteristics, the evolution of their understanding and the questions which still remain open have been widely reviewed in the last five IAU colloquia and symposia on these stars (Slettebak 1976; Jaschek & Groth 1982; Slettebak & Snow 1987; Balona et al. 1994; Smith et al. 2000). The outstanding physical problems related to them can roughly be summarized into two groups of global questions: a) what is the nature of the central stars and when does the Be phenomenon occur during their evolutionary span?; b) what is the structure of their circumstellar envelopes (CE) and how are they produced? es
dc.format.extent p. 861-882 es
dc.language en es
dc.title High and intermediate-resolution spectroscopy of Be stars es
dc.type Articulo es
sedici.identifier.uri http://www.aanda.org/index.php?option=com_article&access=bibcode&Itemid=129&bibcode=2001A%2526A...378..861CFUL es
sedici.title.subtitle An atlas of H g, He I 4471 and Mg II 4481 lines es
sedici.creator.person Chauville, J. es
sedici.creator.person Zorec, Juan es
sedici.creator.person Ballereau, Dominique es
sedici.creator.person Morrell, Nidia es
sedici.creator.person Cidale, Lydia Sonia es
sedici.creator.person García, A. es
sedici.subject.materias Ciencias Astronómicas es
sedici.subject.descriptores Geofísica, astronomía y astrofísica es
sedici.description.fulltext true es
mods.originInfo.place Facultad de Ciencias Astronómicas y Geofísicas es
sedici.subtype Articulo es
sedici2003.identifier ARG-UNLP-ART-0000006571 es
sedici.relation.journalTitle Astronomy and Astrophysics es
sedici.relation.journalVolumeAndIssue vol. 378, no. 3 es


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