Companion-launched jets and their effect on the dynamics of common envelope interaction simulations

Shiber, Sagiv; Iaconi, Roberto; Marco, Orsola De; Soker, Noam

doi:10.1093/mnras/stz2013

Cited by 83 publications

(66 citation statements)

References 74 publications

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“…Density and outflow velocity of the stellar wind for models with different initial wind velocities at the surface of the AGB star. The pole-to-equator density ratio is also important in the shaping of a hot bubble resulting from the shocked material by a jet from the secondary star, at the RLOF phase (Shiber et al 2019, and references therein). For the above reasons, the density ratio has to be taken into account to study the correct hydrodynamical evolution of the binary system.…”

Section: Discussionmentioning

confidence: 99%

AGB winds in interacting binary stars

Bermúdez-Bustamante

Garcı́a-Segura

Steffen

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We perform numerical simulations to investigate the stellar wind from interacting binary stars. Our aim is to find analytical formulae describing the outflow structure. In each binary system the more massive star is in the asymptotic giant branch and its wind is driven by a combination of pulsations in the stellar surface layers and radiation pressure on dust, while the less massive star is in the main sequence. Time averages of density and outflow velocity of the stellar wind are calculated and plotted as profiles against distance from the centre of mass and colatitude angle. We find that mass is lost mainly through the outer Lagrangian point L 2 . The resultant outflow develops into a spiral at low distances from the binary. The outflowing spiral is quickly smoothed out by shocks and becomes an excretion disk at larger distances. This leads to the formation of an outflow structure with an equatorial density excess, which is greater in binaries with smaller orbital separation. The pole-to-equator density ratio reaches a maximum value of ∼ 10 5 at Roche-Lobe Overflow state. We also find that the gas stream leaving L 2 does not form a circumbinary ring for stellar mass ratios above 0.78, when radiation pressure on dust is taken into account. Analytical formulae are obtained by curve fitting the 2-dimensional, azimuthally averaged density and outflow velocity profiles. The formulae can be used in future studies to setup the initial outflow structure in hydrodynamic simulations of common-envelope evolution and formation of planetary nebulae.

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Section: Discussionmentioning

confidence: 99%

AGB winds in interacting binary stars

Bermúdez-Bustamante

Garcı́a-Segura

Steffen

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…In summary, unless jets play a crucial role in driving CE ejection (e.g., Soker 2015;Shiber et al 2019), our model for the CE outcome and binary survival is optimistic with respect to more realistic assumptions. As such, the expectation that CE ejection in binaries with BH or NS accretors requires RSG donors currently appears quite robust.…”

Section: How Robust Is the Prediction That Ce Evolution In Bhmentioning

confidence: 95%

It has to be cool: Supergiant progenitors of binary black hole mergers from common-envelope evolution

Klencki

Nelemans

Istrate

et al. 2021

A&A

129

122

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Common-envelope (CE) evolution in massive binary systems is thought to be one of the most promising channels for the formation of compact binary mergers. In the case of merging binary black holes (BBHs), the essential CE phase takes place at a stage when the first BH is already formed and the companion star expands as a supergiant. We aim to decipher the kinds of BH binaries with supergiant companions that could potentially evolve through and survive a CE phase. To this end, we compute envelope binding energies from detailed massive stellar models at different evolutionary stages and metallicities. We make multiple physically extreme choices of assumptions that favor easier CE ejection as well as account for recent advancements in mass-transfer stability criteria. We find that even with the most optimistic assumptions, a successful CE ejection in BH binaries is only possible if the donor is a massive convective-envelope giant, namely a red supergiant (RSG). The same is true for neutron-star binaries with massive companions. In other words, pre-CE progenitors of BBH mergers are BH binaries with RSG companions. We find that because of its influence on the radial expansion of massive giants, metallicity has an indirect but a very strong effect on the chemical profile, density structure, and the binding energies of RSG envelopes. Our results suggest that merger rates from population-synthesis models could be severely overestimated, especially at low metallicity. Additionally, the lack of observed RSGs with luminosities above log(L/L⊙) ≈ 5.6 − 5.8, corresponding to stars with M ≳ 40 M⊙, puts into question the viability of the CE channel for the formation of the most massive BBH mergers. Either such RSGs elude detection due to very short lifetimes, or they do not exist and the CE channel can only produce BBH systems with total mass ≲50 M⊙. Finally, we discuss an alternative CE scenario in which a partial envelope ejection is followed by a phase of possibly long and stable mass transfer.

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“…The inflation of these two lobes compresses the equatorial gas (e.g., Akashi & Soker 2008), adding to the action of the gravity of the companion, here a NS, and jets at the onset of the CEE (e.g. Shiber et al 2019). I schematically draw this CSM structure in Fig.…”

Section: Pre-explosion Bipolar Csmmentioning

confidence: 99%

A common envelope jets supernova (CEJSN) impostor scenario for fast blue optical transients

Soker

2022

Preprint

Self Cite

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I propose a new scenario, the polar common envelope jets supernova (CEJSN) impostor scenario, to account for AT2018cow-like fast blue optical transients (FBOTs). The polar CEJSN impostor scenario evolves through four main phases. (1) A red supergiant (RSG) star expands to tidally interact with a neutron star (NS) companion (or a black hole). The interaction increases the RSG mass loss rate to form a circumstellar matter (CSM) halo to r 0.1 pc. (2) Shortly before the onset of a common envelope evolution (CEE) and about a year before explosion the NS accretes mass from the RSG envelope and launches jets that inflate two opposite lobes in the CSM within ≈ 100 AU. (3) The NS-RSG system enters a CEE phase during which the system ejects most of the envelope mass in a dense equatorial outflow. (4) At the termination of the CEE the leftover envelope forms a circumbinary disk around the NS-core system. The NS accretes mass from the circumbinary disk and launches energetic jets that when collide with the fronts of the CSM lobes power an FBOT event. The low mass of the jets-lobes interaction zones and their large distance, of about 100 AU, from the center account for the fast transient. In the future the core collapses to form a second NS. In the far future the two NS might merge. I suggest that FBOTs and similar fast transients are CEJSN impostors which compose a large fraction of the progenitors of NS-NS merger binaries.

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Companion-launched jets and their effect on the dynamics of common envelope interaction simulations

Cited by 83 publications

References 74 publications

AGB winds in interacting binary stars

AGB winds in interacting binary stars

It has to be cool: Supergiant progenitors of binary black hole mergers from common-envelope evolution

A common envelope jets supernova (CEJSN) impostor scenario for fast blue optical transients

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