Common envelope events with low-mass giants: understanding the energy budget

Nandez, Jose L. A.; Іванова, Наталя

doi:10.1093/mnras/stw1266

Cited by 83 publications

(66 citation statements)

References 23 publications

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“…We will analyze the energetics of gas in the simulation domain extensively in what follows (see Nandez & Ivanova 2016, for a similar analysis of the energetics of particle-hydrodynamic simulations of binary interaction). In our simulated system, we evaluate the specific binding energy of material using the Bernoulli parameter,…”

Section: Numerical Methods and Simulationsmentioning

confidence: 99%

Bound Outflows, Unbound Ejecta, and the Shaping of Bipolar Remnants during Stellar Coalescence

MacLeod

Ostriker

Stone

2018

ApJ

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Recent observations have revealed that the remnants of stellar-coalescence transients are bipolar. This raises the questions of how these bipolar morphologies arise and what they teach us about the mechanisms of mass ejection during stellar mergers and common-envelope phases. In this paper, we analyze hydrodynamic simulations of the lead-in to binary coalescence, a phase of unstable Roche lobe overflow that takes the binary from the Roche limit separation to the engulfment of the more compact accretor within the envelope of the extended donor. As mass transfer runs away at increasing rates, gas trails away from the binary. Contrary to previous expectations, early mass loss from the system remains bound to the binary and forms a circumbinary torus. Later ejecta, generated as the accretor grazes the surface of the donor, have very different morphologies and are unbound. These two components of mass loss from the binary interact as later, higher-velocity ejecta collide with the circumbinary torus formed by earlier mass loss. Unbound ejecta are redirected toward the poles, and escaping material creates a bipolar outflow. Our findings show that the transition from bound to unbound ejecta from coalescing binaries can explain the bipolar nature of their remnants, with implications for our understanding of the origin of bipolar remnants of stellar-coalescence transients and, perhaps, some preplanetary nebulae.

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Section: Numerical Methods and Simulationsmentioning

confidence: 99%

Bound Outflows, Unbound Ejecta, and the Shaping of Bipolar Remnants during Stellar Coalescence

MacLeod

Ostriker

Stone

2018

ApJ

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“…The complexities of CEE are less uncertain than they used to be, as a result of extensive hydrodynamic simulations in recent years (e.g. Passy et al, 2012;Ricker & Taam, 2012;Nandez & Ivanova, 2016;Ohlmann et al, 2016;Staff et al, 2016;Iaconi et al, 2017), although this work focuses on low mass (∼1-2 M ⊙ ) giants. However, while our straight-forward binding/orbital energy prescription for CEE provides results in line with current thinking, how best to model the CEE phase within a 1D hydrostatic evolution code is still unclear (Ivanova et al, 2013).…”

Section: Roche Lobe Overflow Common Envelope Evolution and Mergersmentioning

confidence: 99%

Binary Population and Spectral Synthesis Version 2.1: Construction, Observational Verification, and New Results

Eldridge

Stanway

Xiao

et al. 2017

Publ. Astron. Soc. Aust.

878

727

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The Binary Population and Spectral Synthesis (BPASS) suite of binary stellar evolution models and synthetic stellar populations provides a framework for the physically motivated analysis of both the integrated light from distant stellar populations and the detailed properties of those nearby. We present a new version 2.1 data release of these models, detailing the methodology by which BPASS incorporates binary mass transfer and its effect on stellar evolution pathways, as well as the construction of simple stellar populations. We demonstrate key tests of the latest BPASS model suite demonstrating its ability to reproduce the colours and derived properties of resolved stellar populations, including wellconstrained eclipsing binaries. We consider observational constraints on the ratio of massive star types and the distribution of stellar remnant masses. We describe the identification of supernova progenitors in our models, and demonstrate a good agreement to the properties of observed progenitors. We also test our models against photometric and spectroscopic observations of unresolved stellar populations, both in the local and distant Universe, finding that binary models provide a self-consistent explanation for observed galaxy properties across a broad redshift range. Finally, we carefully describe the limitations of our models, and areas where we expect to see significant improvement in future versions.

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“…Although recent studies of the common envelope evolution (CEE) reveal many properties of the binary interaction and its outcomes (e.g., Passy et al 2012;Ricker & Taam 2012;Ohlmann et al 2016;Nandez & Ivanova 2016;Kuruwita et al 2016;Chamandy et al 2018;Glanz & Perets 2018;Iaconi et al 2018;MacLeod et al 2018a,b;Chamandy et al 2019;Michaely & Perets 2019;Reichardt et al 2019;Wilson & Nordhaus 2019;, there are still many open questions. Two open questions are how to calculate the final orbital separation and at what conditions the companion launches jets.…”

Section: Introductionmentioning

confidence: 99%

The class of supernova progenitors that result from fatal common envelope evolution

Soker

2019

Sci. China Phys. Mech. Astron.

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I construct the class of supernovae and supernova progenitors that result from fatal common envelope evolution (CEE). The fatal CEE progenitors are stellar binary systems where a companion spirals-in inside the envelope of a giant star and merges with the core. The companion can be a neutron star (NS; or a black hole) that destroys the core and by that forms a common envelope jets supernova (CEJSN), a white dwarf (WD) that merges with the core to form a massive WD that later might explode as a Type Ia supernova (the core degenerate scenario), or a main sequence companion. In the latter case the outcome might be a core collapse supernova (CCSN) of a blue giant, a CCSN of type IIb or of type Ib. In another member of this class two giant stars merge and the two cores spiral-in toward each other to form a massive core that later explodes as a CCSN with a massive circumstellar matter (CSM). I discuss the members of this class, their characteristics, and their common properties. I find that fatal CEE events account for ≈ 6 − 10% of all CCSNe, and raise the possibility that a large fraction of peculiar and rare supernovae result from the fatal CEE. The study of these supernova progenitors as a class will bring insights on other types of supernova progenitors, as well as on the outcome of the CEE.

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Common envelope events with low-mass giants: understanding the energy budget

Cited by 83 publications

References 23 publications

Bound Outflows, Unbound Ejecta, and the Shaping of Bipolar Remnants during Stellar Coalescence

Bound Outflows, Unbound Ejecta, and the Shaping of Bipolar Remnants during Stellar Coalescence

Binary Population and Spectral Synthesis Version 2.1: Construction, Observational Verification, and New Results

The class of supernova progenitors that result from fatal common envelope evolution

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