Ultraviolet Spectroscopy of R Arae: An Active Interacting Binary

Details Ultraviolet Spectroscopy of R Arae: An Active Interacting Binary Ultraviolet Spectroscopy of R Arae: An Active Interacting Binary

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.0331r&link_type=abstract

American Astronomical Society, AAS Meeting #211, #03.31; Bulletin of the American Astronomical Society, Vol. 39, p.728

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The eclipsing, interacting binary star system R Arae (HD149730) is in a very active and very rare stage of its evolution. After receiving some attention in the 1980s and early 1990s, R Ara has unfortunately been neglected. A total of 124 high resolution ultraviolet spectra (taken by the IUE satellite) are analyzed. The data taken in September of 1989 are especially of interest considering that there are 36 consecutive spectra that span the entire 4.4-day orbital period. R Ara is believed to consist of a B9 primary and an unknown (early F to K ?) secondary, and is engulfed in a thick, nebulous plasma resulting from rapid mass flow within and from the system. Several light curves spanning the UV region were generated. In addition to continuum flux levels and radial velocities, the results of photometric and spectroscopic analyses are presented. These studies reveal clues about the construction of this interacting binary (mass flow direction, high temperature regions, etc.) and help to identify its evolutionary status. There is a peculiar but consistent apparent "eclipse” past phase 0.5, as well as another consistent minimum at around first quadrature. Non-orbital gas motions are observed, with Mg II and Si IV exhibiting clear gas stream effects. R Ara is most likely at the end of its first phase of rapid mass transfer, on its way to becoming a classic Algol-type system.

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