Wind Collision and Accretion Simulations of the Massive Binary System HD 166734

Abstract

We run hydrodynamic simulations which follow the colliding winds structure of the massive binary system HD 166734 along its binary orbit, and show that close to periastron passage the secondary wind is suppressed and the secondary accretes mass from the primary wind. The system consists two blue supergiants with masses of $M_1\approx 39.5{\mathrm{M}}_{\odot }$ and $M_2\approx 30.5{\mathrm{M}}_{\odot }$, on a $P\simeq 34.538\mathrm{days}$ orbit with eccentricity of $e\approx 0.618$. This close O-O binary with high eccentricity is observed through its orbit in the X-rays, where it shows an unusual long minimum close to periastron passage. We use advanced simulations with wind acceleration and prescription treatment of accretion and simulate the entire orbit at high resolution that captures the instabilities in the winds. We find that the colliding wind structure is unstable even at apastron. As the stars approach periastron passage the secondary wind is quenched by the primary wind and the accretion onto the secondary begins. The accretion phase lasts for $\simeq 12\mathrm{days}$, and the amount of accreted mass per cycle we obtain is $M_{\mathrm{acc}}\simeq 1.3\cdot 10^{-8}{\mathrm{M}}_{\odot }$. The accretion phase can account for the observed decline in X-ray emission from the system.

arXiv commentAccepted to MNRAS

References in corpus (28)

• Binary interaction dominates the evolution of massive stars
• Mass loss from hot massive stars
• Southern Massive Stars at High Angular Resolution: Observational Campaign and Companion Detection
• A Review of Bondi--Hoyle--Lyttleton Accretion
• Nonlinear Instabilities in Shock-Bounded Slabs
• The masses, and the mass discrepancy of O-type stars
• A consistent solution for the velocity field and mass-loss rate of massive stars
• A multispectral view of the periodic events in eta Carinae
• Very Massive Stars in the Local Universe
• Massive star evolution : rotation, winds, and overshooting vectors in the Mass-Luminosity plane I. A calibrated grid of rotating single star models
• Possible Implications of Mass Accretion in Eta Carinae
• Accretion by the Secondary in Eta Carinae During the Spectroscopic Event: I. Flow Parameters
• Suppression of X-rays from radiative shocks by their thin-shell instability
• Accretion onto the Companion of Eta Carinae During the Spectroscopic Event: II. X-Ray Emission Cycle
• Eta Carinae's 2014.6 Spectroscopic Event: Clues to the Long-term Recovery from its Great Eruption
• Understanding the X-ray Flaring from Eta Car
• Investigating the X-ray emission from the massive WR+O binary WR 22 using 3D hydrodynamical models
• Simulations of the non-linear thin shell instability
• Using X-Ray Observations to Explore the Binary Interaction in Eta Carinae
• A modern study of HD166734: a massive supergiant system
• The Binarity of Eta Carinae and its Similarity to Related Astrophysical Objects
• Accretion onto the Companion of Eta Carinae During the Spectroscopic Event. IV. the Disappearance of Highly Ionized Lines
• The chaotic wind of WR 40 as probed by BRITE
• Eta Carinae's Thermal X-ray Tail Measured with XMM-Newton and NuSTAR
• Accretion at the periastron passage of Eta Carinae
• Simulating the Response of the Secondary Star of Eta Carinae to Mass Accretion at Periastron Passage
• The X-ray Lightcurve of the Supermassive star eta Carinae, 1996--2014
• An X-ray view of HD166734, a massive supergiant system

Cited by in corpus (2)

• Investigation of the nature of the wind interaction in HD93205 based on multi-epoch X-ray observations
• Accretion in massive colliding wind binaries and the effect of wind momentum ratio