Long-term monitoring of θ1 Ori C: The spectroscopic orbit and an improved rotational period

Abstract

Context. The young O-type star Ori C, the brightest star of the Trapezium cluster in Orion, is one of only two known magnetic rotators among the O stars. However, not all spectroscopic variations of this star can be explained by the magnetic rotator model. We present results from a long-term monitoring to study these unexplained variations and to improve the stellar rotational period.Aims. We want to study long-term trends of the radial velocity of Ori C, to search for unusual changes, to improve the established rotational period and to check for possible period changes.Methods. We combine a large set of published spectroscopic data with new observations and analyze the spectra in a homogeneous way. We study the radial velocity from selected photo-spheric lines and determine the equivalent width of the Hα and Heii lines.Results. We find evidence for a secular change of the radial velocity of Ori C that is consistent with the published interferometric orbit. We refine the rotational period of Ori C and discuss the possibility of detecting period changes in the near future. © 2008 ESO.