H-BETA LINE-PROFILE VARIABILITY OF 7 SOUTHERN BE STARS

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dc.contributor.authorMENNICKENT, RE
dc.date.accessioned2025-01-23T19:22:43Z
dc.date.available2025-01-23T19:22:43Z
dc.date.issued1991
dc.description.abstractThe results of spectroscopic observations of six B0-B4e and one B7e stars at the Manuel Foster Observatory (Chile) during 1984-87 are reported. By means of photographic spectroscopy (20 angstrom/mm), equivalent widths, peak separations and V/R ratios were obtained for a total of 106 H-beta and 7 H-gamma line profiles. Emission episodes in H-beta were detected in 27 CMa and lambda Pav, lasting at least 5 months and 18 days respectively. Significant variations in the equivalent width of the H-beta emission line, W-beta, in time scales of months were found in kappa CMa, PP Car and QY Car. On the other hand alpha Ara and member-of PsA showed a relatively constant strength of emission. The variations in W-beta were interpreted as the cumulative effect of several individual ejections from the stellar surface with mass loss rates of the order of 10(-10) M./yr. A variable, centrally detached, disk-type H-beta emitting region with extensions r-beta less-than-or-equal-to 5r* and rotation law v(r) approximately 1/r, which implies outflow or inflow of matter rather than a stable Keplerian disk, was derived by comparing emission line profile data of all stars.
dc.fuente.origenWOS
dc.identifier.issn0365-0138
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/99090
dc.identifier.wosidWOS:A1991FE60600001
dc.issue.numero1
dc.language.isoen
dc.pagina.final18
dc.pagina.inicio1
dc.revistaAstronomy & astrophysics supplement series
dc.rightsacceso restringido
dc.subjectBE STARS
dc.subjectSPECTROSCOPY
dc.subjectEMISSION LINES
dc.titleH-BETA LINE-PROFILE VARIABILITY OF 7 SOUTHERN BE STARS
dc.typeartículo
dc.volumen88
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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