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The nature of the line profile variability in the spectrum of the massive binary HD 152219

机译：大规模二进制HD 152219频谱中的线轮廓可变性的性质

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Context. HD 152219 is a massive binary system with O9.5III+ B1-2V/IIIcomponents and a short orbital period of 4.2d. Its primary component further displays clear line profile variability (LPV). The primary component being located within the pulsational instability domain predicted for high-luminosity stars, we previously suggested that the observed LPV could be associated with non-radial pulsations. Aims. The aim of the present work is to determine the nature of the observed LPV in the spectrum of the primary component of HD152219. Methods. During a 4-night FEROS monitoring campaign, we collected a new set of 134high signal-to-noise spectra. These new observations were then used to re-investigate the variability of different line profiles in the spectrum of HD152219. Results. Based on the present analysis, we discard the non-radial pulsations and point out the Rossiter-McLaughlin effect as the cause of the LPV in HD152219. The upper limit on the amplitude of possible weak pulsations is set at a few parts per thousand of the continuum level. Key words: stars: individual: HD 152219 - stars: oscillations - binaries: close - binaries: spectroscopic - stars: early-type - line: profiles
机译：上下文。 HD 152219是由O9.5III + B1-2V / III组分组成的大型双星系统，轨道周期为4.2d。其主要组成部分还显示清晰的线轮廓变异性（LPV）。主要成分位于为高光度恒星预测的脉动不稳定性域内，我们之前曾建议观察到的LPV可能与非径向脉动有关。目的本工作的目的是确定HD152219的主要成分频谱中观察到的LPV的性质。方法。在为期4夜的FEROS监视活动中，我们收集了一组新的134个高信噪比频谱。这些新的观察结果随后被用于重新调查HD152219光谱中不同谱线的变异性。结果。基于目前的分析，我们丢弃了非径向脉动，并指出Rossiter-McLaughlin效应是HD152219中LPV的原因。可能的弱脉动幅度的上限设置为连续千分之一水平的几分之一。关键词：恒星：个人：HD 152219-恒星：振荡-双星：关闭-双星：光谱-恒星：早期类型-线：轮廓

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