New light on the multiple jets of CRL 618

Riera, A.; Velázquez, P. F.; Raga, A. C.; Estalella, R.; Castrillón, A.

doi:10.1051/0004-6361/201321946

Cited by 14 publications

(29 citation statements)

References 48 publications

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“…Additionally, we impose a linear trend of decreasing ejection velocity with time in order to reproduce the observed behavior of the proper motion velocity (Riera et al 2014).…”

Section: Model Assumptionsmentioning

confidence: 99%

“…In contrast to the scenario explored by Riera et al (2014), in this work we consider an "asymmetrical jet-ejection mechanism" that is inspired by the results of Montgomery (2012) and Fendt & Sheikhnezami (2013). The first of these papers presents a numerical study (by means of smoothed particle hydrodynamics simulations) of precessing accretion disks.…”

Section: Model Assumptionsmentioning

confidence: 99%

“…In Equations (3)- (4), t sup indicates the duration of the superwind phase, i.e., the time during which the star ejects a slow but higher mass-loss rate wind, while t trans is the transition time between the AGB wind phase (at a lower mass-loss rate) and the superwind phase (Mellema 1995). Both t sup and t trans were chosen to be 400 yr (Sánchez Contreras et al 2002;Riera et al 2014). The densities ρ AGB and ρ sup are calculated as…”

Section: Initial Setup Of the Numerical Simulationmentioning

confidence: 99%

“…The pPN CRL 618 exhibits a four-lobe mirror-symmetric morphology with respect to a plane perpendicular to fingers labeled J1 and J1 by Riera et al (2014). 4 Numerical simulations have been carried out in the past with the intent of reproducing both the morphology and kinematics of this pPNs, such as the study of , who proposed a scenario in which a CFW is interacting with a spherical AGB wind (see also Lee et al 2009).…”

Section: Introductionmentioning

confidence: 99%

“…While the numerical model is based on the work of Velázquez et al (2013), a time-decreasing trend was added to the jet velocity in the model description in order to guarantee consistency with the proper motion determined observationally by Riera et al (2014). Despite of this, they obtain point-symmetric morphologies in their synthetic maps.…”

Section: Introductionmentioning

confidence: 99%

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An Asymmetric Jet-Launching Model for the Protoplanetary Nebula CRL 618

Velázquez

Riera

Raga

et al. 2014

ApJ

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We propose an asymmetrical jet-ejection mechanism in order to model the mirror symmetry observed in the lobe distribution of some protoplanetary nebulae (pPNs), such as the pPN CRL 618. Three-dimensional hydrodynamical simulations of a precessing jet launched from an orbiting source were carried out, including an alternation in the ejections of the two outflow lobes, depending on which side of the precessing accretion disk is hit by the accretion column from a Roche lobe-filling binary companion. Both synthetic optical emission maps and position-velocity diagrams were obtained from the numerical results with the purpose of carrying out a direct comparison with observations. Depending on the observer's point of view, multipolar morphologies are obtained that exhibit a mirror symmetry at large distances from the central source. The obtained lobe sizes and their spatial distributions are in good agreement with the observed morphology of the pPN CRL 618. We also obtain that the kinematic ages of the fingers are similar to those obtained in the observations.

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“…Additionally, we impose a linear trend of decreasing ejection velocity with time in order to reproduce the observed behavior of the proper motion velocity (Riera et al 2014).…”

Section: Model Assumptionsmentioning

confidence: 99%

Section: Model Assumptionsmentioning

confidence: 99%

Section: Initial Setup Of the Numerical Simulationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

An Asymmetric Jet-Launching Model for the Protoplanetary Nebula CRL 618

Velázquez

Riera

Raga

et al. 2014

ApJ

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Pre-planetary nebulae: a context for principles, progress, and questions on how binaries and magnetic fields produce jets

Blackman

2020

Proc. IAU

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Astrophysical outflows treated initially as spherically symmetric often show evidence for asymmetry once seen at higher resolution. The preponderance of aspherical and multipolar planetary nebulae (PN) and pre-planetary nebulae (PPN) was evident after many observations from the Hubble Space Telescope. Binary interactions have long been thought to be essential for shaping asymmetric PN/PPN, but how? PPN are the more kinematically demanding of the two, and warrant particular focus. I address how progress from observation and theory suggests two broad classes of accretion driven PPN jets: one for wider binaries (PPN-W) where the companion is outside the outer radius of the giant and accretes via Roche lobe overflow, and the other which occurs in the later stages of CE for close binaries (PPN-C). The physics within these scenarios connects to progress and open questions about the role and origin of magnetic fields in the engines and in astrophysical jets more generally.

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The Emerging Planetary Nebula CRL 618 and Its Unsettled Central Star(s)

Balick

Riera

Raga

et al. 2014

ApJ

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We report deep long-slit emission-line spectra, the line flux ratios, and Doppler profile shapes of various bright optical lines. The low-ionization lines (primarily [N I], [O I], [S II], and [N II]) originate in shocked knots, as reported by many previous observers. Dustscattered lines of higher ionization are seen throughout the lobes but do not peak in the knots. Our analysis of these line profiles and the readily discernible stellar continuum shows that (1) the central star is an active symbiotic (whose spectrum resembles the central stars of highly bipolar and young PNe such as M2-9 and Hen2-437) whose compact companion shows a WC8-type spectrum, (2) extended nebular lines of [O III] and He I originate in the heavily obscured nuclear H II region, and (3) the Balmer lines observed throughout the lobes are dominated by reflected Hα emission from the symbiotic star. Comparing our line ratios with those observed historically shows that (1) the [O III]/Hβ and He I/Hβ ratios have been steadily rising by large amounts throughout the nebula, (2) the Hα/Hβ ratio is steadily decreasing while Hγ/Hβ remains nearly constant, and (3) the low-ionization line ratios formed in the shocked knots have been in decline in different ways at various locations. We show that the first two of these results might be expected if the symbiotic central star has been active and if its bright Hα line has faded significantly in the past 20 years.

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New light on the multiple jets of CRL 618

Cited by 14 publications

References 48 publications

An Asymmetric Jet-Launching Model for the Protoplanetary Nebula CRL 618

An Asymmetric Jet-Launching Model for the Protoplanetary Nebula CRL 618

Pre-planetary nebulae: a context for principles, progress, and questions on how binaries and magnetic fields produce jets

The Emerging Planetary Nebula CRL 618 and Its Unsettled Central Star(s)

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