Planetary Nebulae Shaped By Common Envelope Evolution

Frank, Adam; Chen, Zhuo; Reichardt, Thomas A.; Marco, Orsola De; Blackman, Eric; Nordhaus, Jason

doi:10.48550/arxiv.1807.05925

Cited by 5 publications

(15 citation statements)

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“…If radiation is intercepted by this high opacity material and does accelerate it, it will do so unevenly, likely partaking in the shaping of the envelope. This conclusion may be very relevant for planetary nebula formation and shaping and add to the complexity of shaping post-CE planetary nebulae already studied by García-Segura et al ( 2018) and Frank et al (2018).…”

Section: Possible Dusty Shell Formationsupporting

confidence: 68%

The impact of recombination energy on simulations of the common-envelope binary interaction

Reichardt

Marco

Iaconi

et al. 2020

Monthly Notices of the Royal Astronomical Society

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During the common envelope binary interaction, the expanding layers of the gaseous common envelope recombine and the resulting recombination energy has been suggested as a contributing factor to the ejection of the envelope. In this paper we perform a comparative study between simulations with and without the inclusion of recombination energy. We use two distinct setups, comprising a 0.88-M and a 1.8-M giants, that have been studied before and can serve as benchmarks. In so doing we conclude that (i) the final orbital separation is not affected by the choice of equation of state. In other words, simulations that unbind but a small fraction of the envelope result in similar final separations to those that, thanks to recombination energy, unbind a far larger fractions. (ii) The adoption of a tabulated equation of state results in a much greater fraction of unbound envelope and we demonstrate the cause of this to be the release of recombination energy. (iii) The fraction of hydrogen recombination energy that is allowed to do work should be about half of that which our adiabatic simulations use. (iv) However, for the heavier star simulation we conclude that it is helium and not hydrogen recombination energy that unbinds the gas and we determine that all helium recombination energy is thermalised in the envelope and does work. (v) The outer regions of the expanding common envelope are likely to see the formation of dust. This dust would promote additional unbinding and shaping of the ejected envelope into axisymmetric morphologies.

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Section: Possible Dusty Shell Formationsupporting

confidence: 68%

The impact of recombination energy on simulations of the common-envelope binary interaction

Reichardt

Marco

Iaconi

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…García-Segura et al (2018) have recently studied the hydrodynamic shaping of stellar winds into planetary nebulae using 2D simulations initialized with the ejecta properties of a previous common-envelope simulation. Frank et al (2018) report a qualitatively similar calculation in 3D. Other theoretical suggestions have focused on the conversion of accretion energy into jets (Soker & Livio 1994;Soker & Kashi 2012;Akashi & Soker 2013;Soker 2015;Akashi et al 2015;Shiber & Soker 2018;Chamandy et al 2018).…”

Section: The Uncertain Origin Of Bipolar Planetary Nebulaementioning

confidence: 55%

“…Other theoretical suggestions have focused on the conversion of accretion energy into jets (Soker & Livio 1994;Soker & Kashi 2012;Akashi & Soker 2013;Soker 2015;Akashi et al 2015;Shiber & Soker 2018;Chamandy et al 2018). As emphasized by Frank et al (2018), the emergent bipolar signatures of these models are tantalizing potential explanations of planetary nebulae morphologies.…”

Section: The Uncertain Origin Of Bipolar Planetary Nebulaementioning

confidence: 99%

“…More recently, several numerical experiments have examined similar gas dynamics in the context of commonenvelope binary systems (Pejcha et al 2017;García-Segura et al 2018;Frank et al 2018;Reichardt et al 2018). Each of these works examined the interaction of a dense torus with fast, spherical ejecta.…”

Section: Comparison To Related Studiesmentioning

confidence: 99%

“…These authors each considered spherical explosion triggered inside a rotationally-supported torus (presumed to be formed by preceding binary interaction), which results in a collimation of ejecta toward the system's poles. García-Segura et al (2018), Frank et al (2018), Reichardt et al (2018) have recently discussed the interaction of stellar winds with the debris of a common envelope episode, and how this process might contribute to observed bipolar planetary nebulae.…”

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confidence: 99%

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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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Extending common envelope simulations from Roche lobe overflow to the nebular phase

Reichardt

Marco

Iaconi

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We have simulated a common envelope interaction of a 0.88-M , 90-R , red giant branch star and a 0.6-M , compact companion with the smoothed particle hydrodynamics code, phantom, from the beginning of the Roche lobe overflow phase to the beginning of the self-regulated inspiral, using three different resolutions. The duration of the Roche lobe overflow phase is resolution dependent and would lengthen with increased resolution beyond the ∼20 years observed, while the inspiral phase and the post-common envelope separation are largely independent of resolution. Mass transfer rates through the Lagrangian points drive the orbital evolution during the Roche lobe overflow phase, as predicted analytically. The absolute mass transfer rate is resolution dependent, but always within an order of magnitude of the analytical value. Similarly, the gravitational drag in the simulations is close to the analytical approximation. This gives us confidence that simulations approximate reality. The L 2 and L 3 outflow observed during Roche lobe overflow remains bound, forming a circumbinary disk that is largely disrupted by the common envelope ejection. However, a longer phase of Roche lobe overflow and weaker common envelope ejection typical of a more stable binary may result in a surviving circumbinary disk. Finally, we examine the density distribution resulting from the interaction for simulations that include or omit the phase of Roche lobe overflow. We conclude that the degree of stability of the Roche lobe phase may modulate the shape of the subsequent planetary nebula, explaining the wide range of post-common envelope planetary nebula shapes observed.

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Planetary Nebulae Shaped By Common Envelope Evolution

Cited by 5 publications

References 0 publications

The impact of recombination energy on simulations of the common-envelope binary interaction

The impact of recombination energy on simulations of the common-envelope binary interaction

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

Extending common envelope simulations from Roche lobe overflow to the nebular phase

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