Space Velocity and Time Span of Jets in Planetary Nebulae

Guerrero, M. A.; Rechy-García, J. S.; Ortiz, R.

doi:10.3847/1538-4357/ab61fa

Cited by 29 publications

(19 citation statements)

References 101 publications

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“…The expansion velocity of our toroidal structure of order 10-30 km s −1 (Fig. 5f) and the 90 − 130 km s −1 bipolar outflow are broadly consistent with observations of young (proto-)PNe and post-AGB stars (Imai et al 2002;Tafoya et al 2020;Guerrero et al 2020). This shows that our proposed mechanism self-consistently reproduces the structures observed in such systems.…”

Section: Comparison To Observationssupporting

confidence: 88%

“…This suggests that at least a large fraction of PNe originates from common-envelope interaction in binary stellar systems, where a star spirals into the envelope of a giant and eventually ejects it (Paczynski 1976;Nordhaus & Blackman 2006;De Marco 2009;Boffin & Jones 2019). Bipolar PNe are often observed to consist of two main components (Sahai & Trauger 1998): a toroidal structure of slowly expanding gas (≈ 20 km s −1 ) and a perpendicular, fast bipolar (sometimes jet-like) outflow (≈ 70 km s −1 , in many cases exceeding 100 km s −1 , see Imai et al 2002;Tafoya et al 2020;Guerrero et al 2020). Magnetic fields have been inferred in such bipolar outflows, e.g., from synchrotron emission (Perez-Sanchez et al 2013), dust continuum polarization (Sabin et al 2015) and maser emission (Miranda et al 2001), and are thought to help collimate them (Vlemmings et al 2006).…”

Section: Introductionmentioning

confidence: 99%

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Bipolar planetary nebulae from common envelope evolution of binary stars

Ondratschek,

Roepke,

Schneider

et al. 2021

Preprint

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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 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: Comparison To Observationssupporting

confidence: 88%

Section: Introductionmentioning

confidence: 99%

Bipolar planetary nebulae from common envelope evolution of binary stars

Ondratschek,

Roepke,

Schneider

et al. 2021

Preprint

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“…It is therefore more reasonable to suppose that the knots were directly ejected as dense bullets from the central star system, in which case the measured mass loss rate is a true reflection of the mass loss in the collimated outflow. Guerrero et al (2020) studied the kinematics of jets in a sample of 58 planetary nebulae. They found that the observed distribution of radial velocities can be reproduced by a bimodal distribution of threedimensional space velocities: 70% of nebulae have low-velocity jets with 𝑉 = (66 ± 26) km s −1 , while 30% have high-velocity jets with 𝑉 = (180 ± 60) km s −1 .…”

Section: Lobes and Knotsmentioning

confidence: 99%

The five axes of the Turtle: symmetry and asymmetry in NGC 6210

Henney,

López,

García-Díaz

et al. 2020

Preprint

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We carry out a comprehensive kinematic and morphological study of the asymmetrical planetary nebula: NGC 6210, known as the Turtle. The nebula's spectacularly chaotic appearance has led to proposals that it was shaped by mass transfer in a triple star system. We study the three-dimensional structure and kinematics of its shells, lobes, knots, and haloes by combining radial velocity mapping from multiple long-slit spectra with proper motion measurements from multi-epoch imaging. We find that the nebula has five distinct ejection axes. The first is the axis of the bipolar, wind-blown inner shell, while the second is the axis of the lop-sided, elliptical, fainter, but more massive intermediate shell. A further two axes are bipolar flows that form the point symmetric, high-ionization outer lobes, all with inclinations close to the plane of the sky. The final axis, which is inclined close to the line of sight, traces collimated outflows of low-ionization knots. We detect major changes in outflow directions during the planetary nebula phase, starting at or before the initial ionization of the nebula 3500 years ago. Most notably, the majority of redshifted low-ionization knots have kinematic ages greater than 2000 years, whereas the majority of blueshifted knots have ages younger than 2000 years. Such a sudden and permanent 180-degree flip in the ejection axis at a relatively late stage in the nebular evolution is a challenge to models of planetary nebula formation and shaping.

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“…Since the early evidence for and detection of jets in planetary nebulae (PNe) (Feibelman 1985;Gieseking et al 1985;Miranda & Solf 1990;López et al 1993), a number of studies have expanded upon the idea that jets in PNe and proto-planetary nebulae (PPNe) are common instead of something exotic, especially after observations made with the Hubble Space Telescope (Borkowski et al 1997;Sahai & Trauger 1998) and ground-based CO millimeter observations (Alcolea et al 2000;Bujarraval et al 2001), which more recently include the Atacama Large Millimeter Array (ALMA) (Sánchez-Contreras et al 2018;Tafoya et al 2020). The list of studies is large, and a recent compilation is given in Guerrero et al (2020).…”

Section: Introductionmentioning

confidence: 99%

Common Envelope Shaping of Planetary Nebulae. III. The Launching of Jets in Proto-Planetary Nebulae

Garcia-Segura,

Taam,

Ricker

2021

Preprint

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We compute successfully the launching of two magnetic winds from two circumbinary disks formed after a common envelope event. The launching is produced by the increase of magnetic pressure due to the collapse of the disks. The collapse is due to internal torques produced by a weak poloidal magnetic field. The first wind can be described as a wide jet, with an average mass-loss rate of ∼ 1.3 × 10 −7 M yr −1 and a maximum radial velocity of ∼ 230 km s −1 . The outflow has a half-opening angle of ∼ 20 • . Narrow jets are also formed intermittently with velocities up to 3,000 km s −1 , with mass-loss rates of ∼ 6 × 10 −12 M yr −1 during short periods of time. The second wind can be described as a wide X-wind, with an average mass-loss rate of ∼ 1.68 × 10 −7 M yr −1 and a velocity of ∼ 30 km s −1 . A narrow jet is also formed with a velocity of 250 km s −1 , and a mass-loss rates of ∼ 10 −12 M yr −1 .The computed jets are used to provide inflow boundary conditions for simulations of proto-planetary nebulae. The wide jet evolves into a molecular collimated outflow within a few astronomical units, producing proto-planetary nebulae with bipolar, elongated shapes, whose kinetic energies reach ∼ 4 × 10 45 erg at 1,000 years. Similarities with observed features in W43A, OH231.8+4.2, and Hen 3-1475 are discussed.The computed wide X-wind produces proto-planetary nebulae with slower expansion velocities, with bipolar and elliptical shapes, and possible starfish type and quadrupolar morphology.

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Space Velocity and Time Span of Jets in Planetary Nebulae

Cited by 29 publications

References 101 publications

Bipolar planetary nebulae from common envelope evolution of binary stars

Bipolar planetary nebulae from common envelope evolution of binary stars

The five axes of the Turtle: symmetry and asymmetry in NGC 6210

Common Envelope Shaping of Planetary Nebulae. III. The Launching of Jets in Proto-Planetary Nebulae

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