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

Abstract

HD 152219 is a massive binary system with O9.5 III + B1-2 V/III components and a short orbital period of 4.2 d. 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. The aim of the present work is to determine the nature of the observed LPV in the spectrum of the primary component of HD 152219.During a 4-night FEROS monitoring campaign, we collected a new set of 134 high signal-to-noise spectra. These new observations were then used to re-investigate the variability of different line profiles in the spectrum of HD 152219. 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 HD 152219. The upper limit on the amplitude of possible weak pulsations is set at a few parts per thousand of the continuum level.

Manuscript accepted for publication in A&A, 5p, 4 figures

References in corpus (2)

• Revised instability domains of SPB and beta Cephei stars
• High resolution optical spectroscopy of Plaskett's star

Cited by in corpus (7)

• Southern Massive Stars at High Angular Resolution: Observational Campaign and Companion Detection
• The massive star binary fraction in young open clusters - II. NGC 6611 (Eagle Nebula)
• A quantitative study of O stars in NGC2244 and the Mon OB2 association
• A new investigation of the binary HD 48099
• Apsidal motion in massive eccentric binaries in NGC 6231: The case of HD 152219
• Eclipsing high-mass binaries I. Light curves and system parameters for CPD-518946, PISMIS24-1 and HD319702
• SALT HRS capabilities for time resolved pulsation analysis: a test with the roAp star $\alpha$ Circini