HST/STIS Ultraviolet Spectroscopy of the Components of the Massive Triple Star delta Ori A

TL;DR

This study uses HST/STIS ultraviolet spectroscopy to spatially resolve and analyze the components of the massive triple star system delta Ori A, providing new insights into their velocities, spectra, and physical properties.

Contribution

First spatially separated UV spectra of delta Ori A's components, enabling detailed analysis of individual star properties and dynamics.

Findings

Detected radial velocities of Aa1 and Ab near velocity extrema.

Tentative evidence for the Aa2 component in spectra.

Compared UV spectra with model spectra to infer stellar parameters.

Abstract

The multiple star system of delta Orionis is one of the closest examples of a system containing a luminous O-type, bright giant star (component Aa1). It is often used as a spectral-type standard and has the highest observed X-ray flux of any hot-star binary. The main component Aa1 is orbited by two lower mass stars, faint Aa2 in a 5.7 day eclipsing binary, and Ab, an astrometric companion with an estimated period of 346 years. Generally the flux from all three stars is recorded in ground-based spectroscopy, and the spectral decomposition of the components has proved difficult. Here we present HST/STIS ultraviolet spectroscopy of delta Ori A that provides us with spatially separated spectra of Aa and Ab for the first time. We measured radial velocities for Aa1 and Ab in two observations made near the velocity extrema of Aa1. We show tentative evidence for the detection of the Aa2 component in cross-correlation functions of the observed and model spectra. We discuss the appearance of the UV spectra of Aa1 and Ab with reference to model spectra. Both stars have similar effective temperatures, but Ab is fainter and is a rapid rotator. The results will help in the interpretation of ground-based spectroscopy and in understanding the physical and evolutionary parameters of these massive stars.