2008
DOI: 10.1111/j.1365-2966.2008.13935.x
|View full text |Cite
|
Sign up to set email alerts
|

Shaping planetary nebulae by light jets

Abstract: We conduct numerical simulations of axisymmetrical jets expanding into a spherical asymptotic giant branch (AGB) slow wind. The three-dimensional flow is simulated with an axially symmetric numerical code. We concentrate on jets that are active for a relatively short time. Our results strengthen other studies that show that jets can account for many morphological features observed in planetary nebulae (PNs). Our main results are as follows. (1) With a single jet's launching episode, we can reproduce a lobe str… Show more

Help me understand this report
View preprint versions

Search citation statements

Order By: Relevance

Paper Sections

Select...
2
1
1
1

Citation Types

4
58
0

Year Published

2008
2008
2023
2023

Publication Types

Select...
8

Relationship

2
6

Authors

Journals

citations
Cited by 45 publications
(62 citation statements)
references
References 49 publications
(97 reference statements)
4
58
0
Order By: Relevance
“…The initial AGB-wind densities employed are always very low (typical values correspond toṀ agb ≈ 10 −6 M yr −1 ) so that thermal pressure is dynamically unimportant (see, e.g., Akashi & Soker 2008). However, as we have mentioned above, typical PN structures require final AGB-wind mass-loss rates of about 10 −4 M yr −1 , higher by about two orders of magnitude than assumed in current jet modelling.…”
Section: Discussionmentioning
confidence: 99%
“…The initial AGB-wind densities employed are always very low (typical values correspond toṀ agb ≈ 10 −6 M yr −1 ) so that thermal pressure is dynamically unimportant (see, e.g., Akashi & Soker 2008). However, as we have mentioned above, typical PN structures require final AGB-wind mass-loss rates of about 10 −4 M yr −1 , higher by about two orders of magnitude than assumed in current jet modelling.…”
Section: Discussionmentioning
confidence: 99%
“…The mass loss rate of the FFS jets and speed were chosen to meet FFS launched by a WD. The SMW jets formed by such FFS jets can have v SMW ≃ 500 km s −1 andṀ SMW ≃ 10 −6 M ⊙ yr −1 , and can lead to the formation of some bipolar PNs (Akashi 2007;Akashi & Soker 2008). As in the previous section I substitute δ = 1.…”
Section: The Constraints On the Fast First Stage (Ffs) Jetsmentioning
confidence: 99%
“…Wide jets were considered (Soker 2004a) and simulated (Akashi 2007;Akashi & Soker 2008) for inflating fat bubbles in PNs in a process similar to that in clusters of galaxies. In some PNs the motion of the nebula is ballistic, i.e., the outflow velocity of different nebular segments is proportional to their distance from the center (e.g., Sanchez Contreras et al 2006).…”
Section: Introductionmentioning
confidence: 99%
“…As a result, instead of spherical fast winds as in the generalized interacting stellar wind (GISW) model (see, e.g., review by Balick & Frank 2002), collimated fast winds (CFWs) have been proposed to operate during the post-AGB phase (and even earlier during the late AGB phase), and be the primary agents for the shaping of PPNs and young PNs (Sahai & Trauger 1998;Sahai 2001). CFW models have been used to account for the morphology and kinematics of a few well-studied PPNs and PNs, with some assuming a radial wind with a small opening angle (Lee & Sahai 2003, hereafter Paper I; Akashi & Soker (2008), some assuming a cylindrical jet either unmagnetized (Cliffe et al 1995;Steffen & López 1998;Guerrero et al 2008) or magnetized (Lee & Sahai 2004), and some assuming a bullet (a massive clump) along the outflow axis (Dennis et al 2008).…”
Section: Introductionmentioning
confidence: 99%