Wind collision and accretion simulations of the massive binary system HD 166734

Kashi, Amit

doi:10.1093/mnras/staa203

Cited by 4 publications

(4 citation statements)

References 55 publications

(52 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Our later simulations in Kashi (2017) included radiation pressure and showed that radiative breaking cannot prevent the accretion, by that confirming the theoretical prediction given by Kashi & Soker (2009c). These simulations in Kashi (2017) are also the first that solve the stars not as point sources but as approximated spheres, allowing directional analysis for accretion. In Kashi (2019) we studied four methods for treating accretion and the response of the accretor to the incoming wind, and found a numerical implementation for treating accretion and wind outflow simultaneously.…”

Section: Introductionsupporting

confidence: 88%

“…Those clumps flow towards the secondary but cannot be decelerated by the ram pressure of the secondary wind and hit the regions from where the secondary wind is launched. Our later simulations in Kashi (2017) included radiation pressure and showed that radiative breaking cannot prevent the accretion, by that confirming the theoretical prediction given by Kashi & Soker (2009c). These simulations in Kashi (2017) are also the first that solve the stars not as point sources but as approximated spheres, allowing directional analysis for accretion.…”

Section: Introductionsupporting

confidence: 88%

“…This might have altered the evolution of both stars (Kashi et al 2016), implying that accretion can play an important role in the evolution and outcome of massive star binaries. The same scenario might have caused other giant eruptions, like the 17 th century eruptions of the prototype Luminous Blue Variable (LBV) star P Cygni (Kashi 2010;Michaelis et al 2018).…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Simulations of Colliding Winds in Massive Binary Systems with Accretion

Kashi

Michaelis

2020

Proc. IAU

View full text Add to dashboard Cite

We run numerical simulations of massive colliding wind binaries, and quantify the accretion onto the secondary under different conditions. We set 3D simulation of a LBV–WR system and vary the LBV mass loss rate to obtain different values of wind momentum ratio η. We show that the mean accretion rate for stationary systems fits a power law Macc∝ η–1.6 for a wide range of η, until for extremely small η saturation in the accretion is reached. We find that the stronger the primary wind, the smaller the opening angle of the colliding wind structure (CWS), and compare it with previous analytical estimates. We demonstrate the efficiency of clumpy wind in penetrating the CWS and inducing smaller scale clumps that can be accreted. We propose that simulations of colliding winds can reveal more relations as the ones we found, and can be used to constrain stellar parameters.

show abstract

Section: Introductionsupporting

confidence: 88%

Section: Introductionsupporting

confidence: 88%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Simulations of Colliding Winds in Massive Binary Systems with Accretion

Kashi

Michaelis

2020

Proc. IAU

View full text Add to dashboard Cite

show abstract

“…Hydrodynamical wind-wind collision studies show that when the wind momentum of one of the stars is significantly larger than that of its companion, a fraction of the shocked wind is accreted (Matsuda et al 1992;Ruffert & Arnett 1994;Nagae et al 2004). Under stationary conditions, the accretion rate is (probably) not sufficient to affect the secondary, but if the incoming stellar wind evolves over time becoming denser and slower, then the numerical simulations find that high density clumps produced by the instabilities in the shocks will fall onto the secondary star (Kashi 2020), potentially leading to non-negligible accretion rates. If such a phenomenon occurred in 1992-1994, the violent expulsion of the material accreted onto Star B could have been responsible for the transitory B1.5Ia + spectrum observed in 1994 and the rapid spectral evolution of the system over the following two years.…”

Section: The 1993-1994 Sudden Eruptionsmentioning

confidence: 99%

Observational Constraints on the Hd 5980 Wind-Wind Collision

Koenigsberger

Morrell

Hillier

et al. 2022

RMxAA

View full text Add to dashboard Cite

Analysis of spectral line profile variations observed over 6 decades in the Wolf-Rayet system HD 5980 lead to the conclusion that Star A, the variable member of the system, has always dominated the wind collision zone (WCZ), contrary to suggestions that before 1994 the stronger wind belonged to its close companion, Star B. The observed variations are caused by a combination of physical occultations, wind eclipses and emission and absorption originating in the WCZ. The effects caused by the leading WCZ branch, which folds around Star B, are clearly seen as it crosses our line of sight to Star A during the secondary eclipse. These effects can inform on the WCZ velocity and density structures. We speculate that differences in line profiles at the same orbital phase but at different epochs may be linked to changes in the WCZ radiative properties. The 2017-2020 spectra indicate that HD 5980 was in a higher activity state than during 2010-2015.

show abstract

Accretion in massive colliding-wind binaries and the effect of the wind momentum ratio

Kashi

Michaelis

Kaminetsky

2022

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We carry out a numerical experiment for ejecting winds in a massive colliding-wind binary system and quantify the accretion on to the secondary star under different primary mass-loss rates. We set a binary system comprising a luminous blue variable (LBV) as the primary and a Wolf–Rayet (WR) star as the secondary, and vary the mass-loss rate of the LBV to obtain different values of the wind momentum ratio η. Our simulations include two sets of cases: one in which the stars are stationary; and one that includes the orbital motion. As η decreases, the colliding-wind structure moves closer to the secondary. We find that for η ≲ 0.05, the accretion threshold is reached and clumps that originate from instabilities are accreted on to the secondary. For each value of η, we calculate the mass accretion rate and identify different regions in the $\dot{M} _{\rm acc}$ – η diagram. For 0.001 ≲ η ≲ 0.05, the accretion is sub-Bondi–Hoyle–Lyttleton (BHL), and the average accretion rate satisfies the power law $\dot{M}_{\rm acc} \propto \eta ^{-1.73}$ for static stars. The accretion is not continuous but rather changes from sporadic to a larger duty cycle as η decreases. For η ≲ 0.001, the accretion becomes continuous in time, and the accretion rate is BHL, up to a factor of 0.4–0.8. The simulations that include the orbital motion give qualitatively similar results, with the steeper power law $\dot{M}_{\rm acc} \propto \eta ^{-1.86}$ for the sub-BHL region and lower η as an accretion threshold.

show abstract

Wind collision and accretion simulations of the massive binary system HD 166734

Cited by 4 publications

References 55 publications

Simulations of Colliding Winds in Massive Binary Systems with Accretion

Simulations of Colliding Winds in Massive Binary Systems with Accretion

Observational Constraints on the Hd 5980 Wind-Wind Collision

Accretion in massive colliding-wind binaries and the effect of the wind momentum ratio

Contact Info

Product

Resources

About