The 218 day period of the peculiar late B-type star HD 101584

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dc.creatorBakker, Eric J.
dc.creatorLamers, Henny J. G. L. M.
dc.creatorWaters, L. B. F. M.
dc.creatorWaelkens, Christoffel
dc.date1995-11-10
dc.date.accessioned2026-07-07T02:20:24Z
dc.date.available2026-07-07T02:20:24Z
dc.descriptionWe have searched for periodicity in the photometric and spectroscopic variations of the enigmatic star HD 101584 and found a long-term variability on a typical time scale of 1700 days (4.7 years) and a highly significant period of 218+-0.7 day. This period is most prominently present in the photometric indices which are a measure for the Balmer jump (Geneva d and Stromgren c). The Doppler velocities of the high-excitation photospheric absorption lines (HeI and CII) seem to be variable with the photometric period. Our data favor the 218 day period for the Doppler velocities with a small probability that the true period is 436 days. We argue that HD 101584 is a close (highly) eccentric 218 day binary system with a low-mass unseen secondary. The photometric and Doppler variations are attributed to changes in the velocity law and mass-loss rate of the stellar wind which lead to asymmetric line profiles and a phase dependent Balmer discontinuity. Binary interaction is responsible for the changes in velocity law and mass-loss rate leading to the observed phenomena.
dc.description13 pages plain latex includes 8 postscript figures, uses psfig.sty; accepted by A&A main journal
dc.identifierhttps://arxiv.org/abs/astro-ph/9511043
dc.identifierhttp://arxiv.org/abs/astro-ph/9511043
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/10201
dc.subjectAstrophysics
dc.titleThe 218 day period of the peculiar late B-type star HD 101584
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