2010/02/25 by R. E. Mennickent, Z. Kolaczkowski, Z. Kołaczkowski +3 · 12 citations
Engineering · Physics and Astronomy · #Astronomical Observations and Instrumentation #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Eclipse #Emission spectrum #Extreme ultraviolet #Optics #Photosphere #Physics #Radial velocity #Spectral energy distribution #Spectral line #Spectrograph #Spectroscopy #Stars #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.1111/j.1365-2966.2010.16588.x
published in Monthly Notices of the Royal Astronomical Society (Oxford University Press) · 13 pages, 14 figures, 7 tables. Accepted for publication in MNRAS, main journal
arxiv created 2010/02/25 · openalex publication_date 2010/04/01 · arxiv updated 2015/05/18 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present high-resolution J-band spectroscopy of V393 Sco obtained with the Cryogenic High-Resolution Infrared Echelle Spectrograph (CRIRES) at the ESO Paranal Observatory along with a discussion of archival International Ultraviolet Explorer (IUE) spectra and published broad-band magnitudes. The best fit to the spectral energy distribution outside eclipse gives K for the gainer, for the donor, mag and a distance of pc, although circumstellar material was not considered in the fit. We argue that V393 Sco is not a member of the open cluster M7. The shape of the He i 1083-nm line shows orbital modulations that can be interpreted in terms of an optically thick pseudo-photosphere mimicking a hot B-type star and relatively large equatorial mass loss through the Lagrangian L3 point during long cycle minimum. IUE spectra show several (usually asymmetric) absorption lines from highly ionized metals and a narrow L emission core on a broad absorption profile. The overall behaviour of these lines suggests the existence of a wind at intermediate latitudes. From the analysis of the radial velocities (RVs) we find M2/M1= 0.24 ± 0.02 and a mass function of f= 4.76 ± 0.24 M. Our observations favour equatorial mass loss rather than high-latitude outflows as the cause for the long variability.