The Kinematics of Point-symmetric Planetary Nebulae

Guerrero, M. A.; Vázquez, R.; López, J. A.

doi:10.1086/300729

Cited by 29 publications

(34 citation statements)

References 17 publications

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“…Another interesting property of observed point-symmetric PNe is that not only the imagery, but also the position-velocity diagrams, show evidence of pointsymmetry (e.g. Guerrero et al 1999;Harman et al 2004), like we find in our synthetic position-velocity diagrams. ) at t = 0 yr (first row), t = 3 yr (second row), t = 6 yr (third row), t = 9 yr (fourth row), and t = 12 yr (fifth row).…”

Section: Comparison With Observationssupporting

confidence: 78%

“…However, many (proto-)PNe have a multipolar or point-symmetric shape (Schwarz 1993;Sahai & Trauger 1998;Guerrero et al 1999;Sahai 1999;Su et al 2003;Harman et al 2004). The nebulae that are formed in the wind-disk interaction would naturally acquire the observed antisymmetry if the disk that confines the fast wind is warped, instead of symmetric under reflection about the equatorial plane.…”

Section: Point-symmetric Nebulaementioning

confidence: 99%

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Blowing up warped disks in 3D

Rijkhorst¹,

Mellema

Icke³

2005

A&A

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The Generalized Interacting Stellar Winds model has been very successful in explaining observed cylindrical and bipolar shapes of planetary nebulae. However, many nebulae have a multipolar or point-symmetric shape. Previous two-dimensional calculations showed that these seemingly enigmatic forms can be reproduced by a two-wind model in which the confining disk is warped, as is expected to occur in irradiated disks. In this paper we present the extension to fully three-dimensional Adaptive Mesh Refinement simulations using the publicly available hydrodynamics package Flash. We briefly describe the mechanism leading to a radiation driven warped disk, and give an equation for its shape. We derive time scales related to the disk and compare them to the radiative cooling time scale of the gas, thereby determining the relevant part of parameter space. By comparing two-dimensional calculations including realistic radiative cooling through a cooling curve, with ones employing a low value for the adiabatic index γ, we show that the latter, computationally less expensive approach, is a valid approximation for treating cooling in our nebulae. The results of the fully three-dimensional wind-disk simulations show our mechanism to be capable of producing a plethora of multipolar (and quadrupolar) morphologies, which can explain the observed shape of a number of (proto-)planetary nebulae.

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Section: Comparison With Observationssupporting

confidence: 78%

Section: Point-symmetric Nebulaementioning

confidence: 99%

Blowing up warped disks in 3D

Rijkhorst¹,

Mellema

Icke³

2005

A&A

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“…In particular, the emission at 0.7 cm has two faint bumps, one toward the north and the other toward the south. These point-symmetric morphologies have been observed in several proto-PNs and PNs (Corradi et al 1993;Guerrero et al 1999;Miranda et al 2001). They have been interpreted as the result of the presence of precessing jetlike winds excavating the slowly expanding envelope ejected during the AGB phase (Miranda et al 2001;Volk et al 2007).…”

Section: Collimated Winds and Tori In Pnsmentioning

confidence: 68%

A Collimated, Ionized Bipolar Structure and a High Density Torus in the Planetary Nebula Iras 17347–3139

Tafoya

Gómez

Patel

et al. 2009

ApJ

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We present observations of continuum (λ = 0.7, 1.3, 3.6, and 18 cm) and OH maser (λ = 18 cm) emission toward the young planetary nebula IRAS 17347−3139, which is one of the three planetary nebulae that are known to harbor water maser emission. From the continuum observations, we show that the ionized shell of IRAS 17347−3139 consists of two main structures: one extended (size ∼1. 5) with bipolar morphology along P.A.= −30• , elongated in the same direction as the lobes observed in the near-infrared (NIR) images, and a central compact structure (size ∼ 0. 25) elongated in the direction perpendicular to the bipolar axis, coinciding with the equatorial dark lane observed in the NIR images. Our image at 1.3 cm suggests the presence of dense walls in the ionized bipolar lobes. We estimate for the central compact structure a value of the electron density at least ∼5 times higher than in the lobes. A high-resolution image of this structure at 0.7 cm shows two peaks separated by about 0. 13 (corresponding to 100-780 AU, using a distance range of 0.8-6 kpc). This emission is interpreted as originating in an ionized equatorial torus-like structure, from whose edges the water maser emission might be arising. We have detected weak OH 1612 MHz maser emission at V LSR ∼ −70 km s −1 associated with IRAS 17347−3139. We derive a 3σ upper limit of < 35% for the percentage of circularly polarized emission. Within our primary beam, we detected additional OH 1612 MHz maser emission in the local standard of rest velocity ranges −5 to −24 and −90 to −123 km s −1 , associated with the sources J17380406−3138387 and OH 356.65−0.15, respectively.

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“…Nevertheless, MHD models have proven to be one of the most promising avenues for advancement in the understanding of the structural development of PNe (see García-Segura et al in these proceedings). Manchado et al (1996) and see Guerrero, Vázquez, & López (1999).…”

Section: The Origin Of Jets In Pnementioning

confidence: 96%

“…There are only twelve PNe formally classified in catalogues as pointsymmetric (Schwarz et al 1993;Manchado et al 1996). However, Guerrero, Vázquez, & López (1999) have pointed out that a certain degree of point-symmetry spans nearly all the morphological groups and evolutionary stages in PNe. This must be considered an important clue to the mass-loss mechanisms during the PN formation process and on the ability of the nebular structure to retain the signatures of point-symmetry at later times.…”

Section: Fliers and Point-symmetric Pnementioning

confidence: 99%

Collimated Outflows in Planetary Nebulae

López¹

2003

Symp. - Int. Astron. Union

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RESUMENNuestro entendimiento sobre la formación de nebulosas planetarias (PNe) ha sido profundamente influenciado en años recientes por la detección de flujos colimados de alta velocidad en estos objetos. Flujos que alcanzan velocidades de expansión de varios cientos de km s −1 así como evidencias de eyecciones múltiples y episódicas, desde la etapa de proto-PNe, han modificado radicalmente nuestros conceptos previos sobre la evolución de objetos post-AGB. Los modelos hidrodinámicos por si solos parecen ahora insuficientes para reproducir muchos de estos fenómenos dinámicos detectados. Modelos MHD y la influencia de núcleos binarios han incrementado su importancia en la interpretación de la diversidad de flujos colimados en PNe. Este trabajo presenta una semblanza de estos fenómenos, y se discute algunos de los retos actuales y tendencias en el campo. ABSTRACTOur understanding of the formation of planetary nebulae (PNe) has been profoundly influenced in recent years by the detection of high-velocity, collimated outflows in these objects. Outflows reaching expansion velocities of several hundred km s −1 and evidences of episodic, multiple ejection events since the proto-PNe stage, have radically modified our previous concepts of the evolution of post-AGB objects. Hydrodynamic models alone seem now incapable of reproducing many of the attendant dynamical phenomena observed in PNe. MHD models and binary nuclei are thus playing an increasingly important role in interpreting the diversity of collimated outflows in PNe. This paper presents an overview of these phenomena and discusses some of the current challenges and trends in the field.

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The Kinematics of Point-symmetric Planetary Nebulae

Cited by 29 publications

References 17 publications

Blowing up warped disks in 3D

Blowing up warped disks in 3D

A Collimated, Ionized Bipolar Structure and a High Density Torus in the Planetary Nebula Iras 17347–3139

Collimated Outflows in Planetary Nebulae

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