Orbital Solution & Fundamental Parameters of sigma Scorpii

Abstract

The first orbital solution for the spectroscopic pair in the multiple star system sigma Scorpii, determined from measurements with the Sydney University Stellar Interferometer (SUSI), is presented. The primary component is of beta Cephei variable type and has been one of the most intensively studied examples of its class. The orbital solution, when combined with radial velocity results found in the literature, yields a distance of 174(+23,-18) pc, which is consistent with, but more accurate than the Hipparcos value. For the primary component we determine 18.4+/-5.4 M_sun, -4.12+/-0.34 mag and 12.7+/-1.8 R_sun for the mass, absolute visual magnitude and radius respectively. A B1 dwarf spectral type and luminosity class for the secondary is proposed from the mass determination of 11.9+/-3.1 M_sun and the estimated system age of 10 Myr.

4 figures, 5 tables, to appear in MNRAS

References in corpus (8)

• A Hipparcos census of the nearby OB associations
• The mass ratio distribution of B-type visual binaries in the Sco OB2 association
• Formation scenarios for the young stellar associations between galactic longitudes l = 280-360 deg
• The Stellar Initial Mass Function
• γ^2 Velorum: Orbital Solution and Fundamental Parameter Determination with SUSI
• Orbital parameters, masses and distance to Beta Centauri determined with the Sydney University Stellar Interferometer and high resolution spectroscopy
• Orbital elements, masses and distance of lambda Scorpii A and B determined with the Sydney University Stellar Interferometer and high resolution spectroscopy
• High-precision elements of double-lined spectroscopic binaries from combined interferometry and spectroscopy. Application to the beta Cephei star beta Centauri

Cited by in corpus (25)

• A Revised Age for Upper Scorpius and The Star-Formation History Among the F-Type Members of the Scorpius-Centaurus OB Association
• Correcting stellar oscillation frequencies for near-surface effects
• Evidence for a Massive Neutron Star from a Radial-Velocity Study of the Companion to the Black Widow Pulsar PSR B1957+20
• Fundamental Properties of Stars using Asteroseismology from Kepler & CoRoT and Interferometry from the CHARA Array
• Asteroseismology and Interferometry
• A Stellar Model-fitting Pipeline for Asteroseismic Data from the Kepler Mission
• The radius and mass of the close solar twin 18 Sco derived from asteroseismology and interferometry
• Automatic Determination of Stellar Parameters via Asteroseismology of Stochastically Oscillating Stars: Comparison with Direct Measurements
• Asteroseismic modelling of the solar-type subgiant star $\beta$ Hydri
• The CubeSpec space mission. I. Asteroseismology of massive stars from time series optical spectroscopy: science requirements and target list prioritisation
• Radii of Rapidly-Rotating Stars, with Application to Transiting-Planet Hosts
• Stellar modelling of Spica, a high-mass spectroscopic binary with a beta Cep variable primary component
• Interstellar extinction and polarization -- A spheroidal dust grain approach perspective
• Lucky Spectroscopy, an equivalent technique to Lucky Imaging. Spatially resolved spectroscopy of massive close visual binaries using the William Herschel Telescope
• Galactic Kinematics from a Sample of Young Massive Stars
• Modelling of Sigma Scorpii, a high-mass binary with a Beta Cep variable primary component
• Substructure, supernovae, and a time-resolved star formation history for Upper Scorpius
• The radius and other fundamental parameters of the F9 V star beta Virginis
• Lucky spectroscopy, an equivalent technique to Lucky Imaging: II. Spatially-resolved intermediate-resolution blue-violet spectroscopy of 19 close massive binaries using the William Herschel Telescope
• Asteroseismic modelling of the solar-like star $\beta$ Hydri
• Investigation of the WR 11 field at decimeter wavelengths
• AMBER/VLTI observations of 5 giant stars
• HP2 Survey V. Ophiuchus: Filament formation in a dispersing cloud complex
• Probing high-mass stellar evolutionary models with binary stars
• New distances for a selected set of visual binaries with inconsistent dynamical masses