Post-common envelope binary systems experiencing helium-shell driven stable mass transfer

Halabi, Ghina M.; Izzard, Robert G.; Tout, Christopher A.

doi:10.1093/mnras/sty2243

Cited by 7 publications

(5 citation statements)

References 61 publications

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“…In our simulations this scenario only occurs in very few systems, demonstrated in Figure 4 by the very low number of systems that undergo a CE event after the first He nova. Further, Halabi et al (2018) demonstrate that stable mass transfer can occur for a wide range of binary parameters in He-shell burning, post-CE binaries. The answer, then, lies elsewhere.…”

Section: He Novaementioning

confidence: 83%

“…The importance of this is that, unlike the HeMS, which often lasts long enough to either merge the stars through inspiral or grow them to 𝑀 Ch , this phase of evolution typically does not. Under the competing influences of core growth and envelope mass loss, these systems often stop mass transferring relatively quickly (Halabi et al 2018), leaving the system in a binary configuration. Further, these systems tend to have wider orbital separations, greatly reducing angular momentum loss through gravitational waves.…”

Section: He Novaementioning

confidence: 99%

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Population synthesis of accreting white dwarfs: rates and evolutionary pathways of H and He novae

Kemp

Karakas

Casey

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Novae are some of the most commonly detected optical transients and have the potential to provide valuable information about binary evolution. Binary population synthesis codes have emerged as the most effective tool for modelling populations of binary systems, but such codes have traditionally employed greatly simplified nova physics, precluding detailed study. In this work, we implement a model treating H and He novae as individual events into the binary population synthesis code binary_c. This treatment of novae represents a significant improvement on the ‘averaging’ treatment currently employed in modern population synthesis codes. We discuss the evolutionary pathways leading to these phenomena and present nova event rates and distributions of several important physical parameters. Most novae are produced on massive white dwarfs, with approximately 70 and 55 per cent of nova events occurring on O/Ne white dwarfs for H and He novae, respectively. Only 15 per cent of H-nova systems undergo a common-envelope phase, but these systems are responsible for the majority of H nova events. All He-accreting He-nova systems are considered post-common-envelope systems, and almost all will merge with their donor star in a gravitational-wave-driven inspiral. We estimate the current annual rate of novae in M31 (Andromeda) to be approximately 41 ± 4 for H novae, underpredicting the current observational estimate of $65^{+15}_{-16}$, and 0.14 ± 0.015 for He novae. When varying common-envelope parameters, the H nova rate varies between 20 and 80 events per year.

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Section: He Novaementioning

confidence: 83%

Section: He Novaementioning

confidence: 99%

Population synthesis of accreting white dwarfs: rates and evolutionary pathways of H and He novae

Kemp

Karakas

Casey

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…A similar scenario was discussed byHalabi, Izzard & Tout (2018) for systems that have gone through common envelope evolution, but this is not thought to be the case for υ Sgr.…”

mentioning

confidence: 79%

Ups!... I did it again: unveiling the hidden companion in Upsilon Sagittarii, a unique binary system at a second mass transfer stage

Gilkis

Shenar

2022

Monthly Notices of the Royal Astronomical Society

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Upsilon Sagittarii is a hydrogen-deficient binary that has been suggested to be in its second stage of mass transfer, after the primary has expanded to become a helium supergiant following core helium exhaustion. A tentative identification of the faint companion in the ultraviolet led to mass estimates of both components that made the helium star in Upsilon Sagittarii a prototypical immediate progenitor of a type Ib/c supernova. However, no consistent model for the complex spectrum has been achieved, casting doubt on this interpretation. In the present study we provide for the first time a composite spectral model that fits the ultraviolet data, and clearly identifies the companion as a rapidly rotating, slowly moving ≈7 M⊙ B-type star, unlike previously suggested. The stripped helium supergiant is less luminous than previous estimates, and with an estimated mass of <1 M⊙ is ruled out as a core-collapse supernova progenitor. We provide a detailed binary evolution scenario that explains the temperature and luminosity of the two components as well as the very low gravity (log g ≈ 1) and extreme hydrogen deficiency of the primary (atmospheric mass fraction XH, 1 ≈ 0.001). The best-fitting model is an intermediate-mass primary (MZAMS, 1 ≈ 5 M⊙) with an initial orbital period of a few days, and a secondary that appears to have gained a significant amount of mass despite its high rotation. We conclude that Upsilon Sagittarii is a key system for testing binary evolution processes, especially envelope stripping and mass accretion.

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“…This seems reasonable because the envelope, even though it is convective, has little enough mass to shrink in response to mass loss, but we admit a more realistic treatment of such phases is currently lacking (cf. Halabi et al 2018).…”

Section: Post-(a)gb and Binary Evolutionmentioning

confidence: 99%

Circumbinary discs for stellar population models

Izzard

Jermyn

2022

Monthly Notices of the Royal Astronomical Society

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We develop a rapid algorithm for the evolution of stable, circular, circumbinary discs suitable for parameter estimation and population synthesis modelling. Our model includes disc mass and angular momentum changes, accretion on to the binary stars, and binary orbital eccentricity pumping. We fit our model to the post-asymptotic giant branch (post-AGB) circumbinary disc around IRAS 08544-4431 finding reasonable agreement despite the simplicity of our model. Our best-fit disc has a mass of about 0.01 M⊙ and angular momentum 2.7 × 1052 g cm2 s−1 ≃ 9M⊙ km s−1 au, corresponding to 0.0079 and 0.16 of the common-envelope mass and angular momentum respectively. The best-fit disc viscosity is αdisc = 5 × 10−3 and our tidal torque algorithm can be constrained such that the inner edge of the disc Rin ∼ 2a. The inner binary eccentricity reaches about 0.13 in our best-fitting model of IRAS 08544-4431, short of the observed 0.22. The circumbinary disc evaporates quickly when the post-AGB star reaches a temperature of ∼6 × 104 K, suggesting that planetismals must form in the disc in about 104 yr if secondary planet formation is to occur, while accretion from the disc on to the stars at ∼10 times the inner-edge viscous rate can double the disc lifetime.

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Post-common envelope binary systems experiencing helium-shell driven stable mass transfer

Cited by 7 publications

References 61 publications

Population synthesis of accreting white dwarfs: rates and evolutionary pathways of H and He novae

Population synthesis of accreting white dwarfs: rates and evolutionary pathways of H and He novae

Ups!... I did it again: unveiling the hidden companion in Upsilon Sagittarii, a unique binary system at a second mass transfer stage

Circumbinary discs for stellar population models

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