Line profile variability in the massive binary HD 152219

Details Line profile variability in the massive binary HD 152219 Line profile variability in the massive binary HD 152219

Jul 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009coast.158..205s&link_type=abstract

"Communications in Asteroseismology, Vol.158, p. 205 Proceedings of "38th Liege International Astrophysical Colloquium: Evoluti

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

HD 152219 is a massive binary system with O9.5 III and B1-2 III/V components and a short orbital period of 4.2 d. In a previous work, we showed that the primary star (M_{prim}˜21 M_&sun;) was presenting clear line profile variabilities (LPVs) that might be caused by nonradial pulsations (NRPs). In the present work, we report on an intensive spectroscopic monitoring, that aimed at unveiling the nature of the detected LPVs. Based on this new data set, we discard the NRPs and point out the Rossiter-McLaughlin effect as % being the cause of the observed LPVs. The upper limit derived on the amplitude of undetected NRPs, if any, is set at a couple of part per thousands of the continuum level.

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