Common Envelope Shaping of Planetary Nebulae. II. Magnetic Solutions and Self-collimated Outflows

Garcı́a-Segura, Guillermo; Taam, Ronald E.; Ricker, P. M.

doi:10.3847/1538-4357/ab8006

Cited by 25 publications

(9 citation statements)

References 40 publications

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“…Ad hoc central engines have been applied in toy models of post-CE systems and demonstrate that such models can indeed reproduce a wide variety of features found in PNe. Suggested engines include enhanced radiation-driven winds (spherically symmetric as well as bipolar; Morris 1981;García-Segura et al 2005;Zou et al 2020), magnetically driven winds (García-Segura et al 2020), and jets launched from a circumbinary disk (Soker & Livio 1994;Garcia-Segura et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Bipolar planetary nebulae from common-envelope evolution of binary stars

Ondratschek

Roepke

Schneider

et al. 2022

A&A

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Asymmetric shapes and evidence for binary central stars suggest a common-envelope origin for many bipolar planetary nebulae. The bipolar components of the nebulae are observed to expand faster than the rest, and the more slowly expanding material has been associated with the bulk of the envelope ejected during the common-envelope phase of a stellar binary system. Common-envelope evolution in general remains one of the biggest uncertainties in binary star evolution, and the origin of the fast outflow has not been explained satisfactorily. We perform three-dimensional magnetohydrodynamic simulations of common-envelope interaction with the moving-mesh code AREPO. Starting from the plunge-in of the companion into the envelope of an asymptotic-giant-branch star and covering hundreds of orbits of the binary star system, we are able to follow the evolution to complete envelope ejection. We find that magnetic fields are strongly amplified in two consecutive episodes: first, when the companion spirals in the envelope and, second, when it forms a contact binary with the core of the former giant star. In the second episode, a magnetically driven, high-velocity outflow of gas is launched self-consistently in our simulations. The outflow is bipolar, and the gas is additionally collimated by the ejected common envelope. The resulting structure reproduces typical morphologies and velocities observed in young planetary nebulae. We propose that the magnetic driving mechanism is a universal consequence of common-envelope interaction that is responsible for a substantial fraction of observed planetary nebulae. Such a mechanism likely also exists in the common-envelope phase of other binary stars that lead to the formation of Type Ia supernovae, X-ray binaries, and gravitational-wave merger events.

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Section: Introductionmentioning

confidence: 99%

Bipolar planetary nebulae from common-envelope evolution of binary stars

Ondratschek

Roepke

Schneider

et al. 2022

A&A

View full text Add to dashboard Cite

show abstract

“…Ad-hoc central engines have been applied in toy models of post-CE systems and demonstrate that such models can indeed reproduce a wide variety of features found in PNe. Suggested engines include enhanced radiation-driven winds (spher-ically symmetric as well as bipolar; Morris 1981;García-Segura et al 2005;Zou et al 2020), magnetically-driven winds (García-Segura et al 2020) and jets launched from a (circumbinary) disk (Soker & Livio 1994;Garcia-Segura et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Bipolar planetary nebulae from common envelope evolution of binary stars

Ondratschek,

Roepke,

Schneider

et al. 2021

Preprint

View full text Add to dashboard Cite

Asymmetric shapes and evidence for binary central stars suggest a common-envelope origin for many bipolar planetary nebulae. The bipolar components of the nebulae are observed to expand faster than the rest and the more slowly expanding material has been associated with the bulk of the envelope ejected during the common-envelope phase of a stellar binary system. Common-envelope evolution in general remains one of the biggest uncertainties in binary star evolution and the origin of the fast outflow has not been explained satisfactorily. We perform three-dimensional magnetohydrodynamic simulations of common-envelope interaction with the moving-mesh code arepo. Starting from the plunge-in of the companion into the envelope of an asymptotic giant branch star and covering hundreds of orbits of the binary star system, we are able to follow the evolution to complete envelope ejection. We find that magnetic fields are strongly amplified in two consecutive episodes. First, when the companion spirals in the envelope and, second, when it forms a contact binary with the core of the former giant star. In the second episode, a magnetically-driven, high-velocity outflow of gas is launched self-consistently in our simulations. The outflow is bipolar and the gas is additionally collimated by the ejected common envelope. The resulting structure reproduces typical morphologies and velocities observed in young planetary nebulae. We propose that the magnetic driving mechanism is a universal consequence of common envelope interaction responsible for a substantial fraction of observed planetary nebulae. Such a mechanism likely also exists in the common-envelope phase of other binary stars that lead to the formation of Type Ia supernovae, X-ray binaries and gravitational-wave merger events.

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“…The non-spherical effects might be very significant at the final CEE phases (e.g., Soker 1992;Reichardt et al 2019;García-Segura et al 2020;Zou et al 2020) and might include the formation of a circumbinary thick disk (e.g., Kashi & Soker 2011;Chen & Podsiadlowski 2017). For that reason, and for neglecting the orbital energy (section 2.4) that increases to non-negligible values at small orbital separations, we do not continue the evolution to late phases when the orbital separation decreases below about a = 20R .…”

Section: Spherical Symmetry and Limited Evolution Timementioning

confidence: 92%

Simulating the negative jet feedback mechanism in common envelope jets supernovae

Grichener,

Cohen,

Soker

2021

Preprint

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We use the stellar evolution code MESA to study the negative jet feedback mechanism in common envelope jets supernovae (CEJSNe) where a neutron star (NS) launches jets in the envelope of a red supergiant (RSG), and find that the feedback reduces the mass accretion rate to be χ j 0.05 − 0.2 times the mass accretion rate without the operation of jets. We mimic the effect of the jets on the RSG envelope by depositing the energy that the jets carry into the envelope zones outside the NS orbit. The energy deposition inflates the envelope, therefore reducing the density in the NS vicinity, which in turn reduces the mass accretion rate in a negative feedback cycle. For the canonical ratio of jets' power to actual accretion power of 0.1, and for results from numerical simulations that show the actual mass accretion rate to be a fraction of 0.1 − 0.5 of the Bondi-Hoyle-Lyttleton mass accretion rate, we find that the negative jet feedback coefficient (the further reduction in the accretion rate) is χ j 0.05 − 0.2, for a NS spiraling-in in the RSG envelope.

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Common Envelope Shaping of Planetary Nebulae. II. Magnetic Solutions and Self-collimated Outflows

Cited by 25 publications

References 40 publications

Bipolar planetary nebulae from common-envelope evolution of binary stars

Bipolar planetary nebulae from common-envelope evolution of binary stars

Bipolar planetary nebulae from common envelope evolution of binary stars

Simulating the negative jet feedback mechanism in common envelope jets supernovae

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