Spectroscopic study of the O-type runaway supergiant HD 195592

Abstract

The scope of this paper is to perform a detailed spectroscopic study of the northern O-type supergiant HD 195592. We use a large sample of high quality spectra in order to investigate its multiplicity, and to probe the line profile variability. Our analysis reveals a clear spectroscopic binary signature in the profile of the He {\sc i} $\lambda$ 6678 line, pointing to a probable O + B system. We report on low amplitude radial velocity variations in every strong absorption line in the blue spectrum of HD 195592. These variations are ruled by two time-scales respectively of 5.063 and about 20 days. The former is firmly established, whilst the latter is poorly constrained. We report also on a very significant line profile variability of the H $\beta$ line, with time scales strongly related to those of the radial velocities. Our results provide significant evidence that HD 195592 is a binary system, with a period that might be the variability time-scale of about 5 days. The second time scale may be the signature of an additional star moving along a wider orbit provided its mass is low enough, even though direct evidence for the presence of a third star is still lacking. Alternatively, the second time-scale may be the signature of a variability intrinsic to the stellar wind of the primary, potentially related to the stellar rotation.

arXiv comment9 pages, 5 postscript figures, accepted for publication in New Astronomy

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Cited by in corpus (6)

• Fermi Large Area Telescope Second Source Catalog
• The Galactic O-Star Spectroscopic Survey. I. Classification System and Bright Northern Stars in the Blue-Violet at R~2500
• Catalogue of particle-accelerating colliding-wind binaries
• Is the bowshock of the runaway massive star HD 195592 a Fermi source?
• Multiplicity of northern bright O-type stars with optical long baseline interferometry
• New self-consistent wind parameters fitting optical spectra of O-type stars observed with HERMES spectrograph