Bubbles in planetary nebulae and clusters of galaxies: Jet properties

Soker, Noam

doi:10.1051/0004-6361:20034120

Cited by 27 publications

(69 citation statements)

References 44 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The possibility that the cavity is excavated (inflated) by the jet itself should also be considered (Soker 2002(Soker , 2004. This would explain the formation of the inner lobes and the rotating pattern.…”

Section: Discussion: Rotating Jet or Light Beam?mentioning

confidence: 99%

The evolution of M 2–9 from 2000 to 2010

Corradi

Balick

Santander-García

2011

A&A

View full text Add to dashboard Cite

Context. Understanding the formation of collimated outflows is one of the most debated and controversial topics in the study of the late stages of stellar evolution. Aims. M 2-9 is an outstanding representative of extreme aspherical flows. It presents unique features such as a pair of high-velocity dusty polar blobs and a mirror-symmetric rotating pattern in the inner lobes. Their study provides important information on the nature of the poorly understood central source of M 2-9 and its nebula. Methods. Imaging monitoring at sub-arcsec resolution of the evolution of the nebula in the past decade is presented. Spectroscopic data provide complementary information. Results. We determine the proper motions of the dusty blobs, which infer a new distance estimate of 1.3 ± 0.2 kpc, a total nebular size of 0.8 pc, a speed of 147 km s −1 , and a kinematical age of 2500 yr. The corkscrew geometry of the inner rotating pattern is confirmed and quantified. Different recombination timescales for different ions explain the observed surface brightness distribution. According to the images taken after 1999, the pattern rotates with a period of 92 ± 4 years. On the other hand, the analysis of images taken between 1952 and 1977 measures a faster angular velocity. If the phenomenon were related to orbital motion, this would correspond to a modest orbital eccentricity (e = 0.10 ± 0.05), and a slightly shorter period (86 ± 5 years). New features have appeared after 2005 on the west side of the lobes and at the base of the pattern. Conclusions. The geometry and travelling times of the rotating pattern support our previous proposal that the phenomenon is produced by a collimated spray of high velocity particles (jet) from the central source, which excites the walls of the inner cavity of M 2-9, rather than by a ionizing photon beam. The speed of such a jet would be remarkable: between 11 000 and 16 000 km s −1 . The rotatingjet scenario may explain the formation and excitation of most of the features observed in the inner nebula, with no need for additional mechanisms, winds, or ionization sources. All properties point to a symbiotic-like interacting binary as the central source of M 2-9. The new distance determination implies system parameters that are consistent with this hypothesis.

show abstract

Section: Discussion: Rotating Jet or Light Beam?mentioning

confidence: 99%

The evolution of M 2–9 from 2000 to 2010

Corradi

Balick

Santander-García

2011

A&A

View full text Add to dashboard Cite

show abstract

“…Therefore, without stating it explicitly, they practically simulated slow-massive-wide jets. For that, it is not surprising that at early times they inflate hot bubbles (Soker 2004a) as in the gasdynamical simulations of wide jets conducted by Sternberg et al (2007). Later in the simulations of Sutherland & Bicknell (2007) the initial jets penetrate the ISM, whereafter they are collimated by the ISM and form narrow jets.…”

Section: Introductionmentioning

confidence: 95%

“…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%

The formation of slow-massive-wide jets

Soker

2008

New Astronomy

View full text Add to dashboard Cite

I propose a model for the formation of slow-massive-wide (SMW) jets by accretion disks around compact objects. This study is motivated by claims for the existence of SMW jets in some astrophysical objects such as in planetary nebulae (PNs) and in some active galactic nuclei in galaxies and in cooling flow clusters. In this model the energy still comes from accretion onto a compact object. The accretion disk launches two opposite jets with velocity of the order of the escape velocity from the accreting object and with mass outflow rate of ∼ 1−20% of the accretion rate as in most popular models for jet launching; in the present model these are termed fast-first-stage (FFS) jets. However, the FFS jets encounter surrounding gas that originates in the mass accretion process, and are terminated by strong shocks close to their origin. Two hot bubbles are formed. These bubbles accelerate the surrounding gas to form two SMW jets that are more massive and slower than the FFS jets. There are two conditions for this mechanism to work. Firstly, the surrounding gas should be massive enough to block the free expansion of the FFS jets. Most efficiently this condition is achieved when the surrounding gas is replenished. Secondly, the radiative energy losses must be small.

show abstract

“…In A2597 both extreme-UV and X-ray observations indicate a mass cooling rate of $50 M yr À1 , which is $0.2 of the value quoted in the past based on ROSAT X-ray observations (see the discussion in Morris & Fabian 2005). Some fraction of the gas may cool to lower temperatures by heat transfer to optical-emitting gas, further reducing the X-ray emission from gas residing at temperatures of T P T min ' 1 keV; the energy transfer can be via mixing (e.g., Oegerle et al 2001;Fabian et al 2001Fabian et al , 2002aJohnstone et al 2002;Bayer-Kim et al 2002) and/or heat conduction Soker 2004b). Intermittent heating, which is part of the moderate CF model, probably occurs by AGN activity.…”

Section: The Proposed Scenariomentioning

confidence: 99%

“…The condition on the opening angle of the jet for that to occur is given by equation (14) of Soker (2004a). We change the variable in that equation as follows.…”

Section: Jet Propagationmentioning

confidence: 99%

Feedback Heating with Slow Jets in Cooling Flow Clusters

Soker¹,

Pizzolato²

2005

ApJ

View full text Add to dashboard Cite

We propose a scenario in which a large fraction or even most of the gas cooling to low temperatures of T < 10 4 K in cooling flow clusters gains energy directly from the central black hole. Most of the cool gas is accelerated to nonrelativistic high velocities, v j ' 10 3 10 4 km s À1 , after flowing through, or close to, an accretion disk around the central black hole. A poorly collimated wind (or a pair of poorly collimated opposite jets) is formed. According to the proposed scenario, this gas inflates some of the X-ray-deficient bubbles, such that the average gas temperature inside these bubbles (cavities) in cooling flow clusters is kT b P 100 keV. A large fraction of these bubbles will be very faint or undetectable in the radio. The bright rims of these weak smaller bubbles will appear as ripples. We suggest that the X-ray ripples observed in the Perseus cluster, for example, are not sound waves but rather the rims of radio-faint weak bubbles that are only slightly hotter than their environment. This scenario is incorporated into the moderate cooling flow model; although not a necessary ingredient in that model, it brings it to better agreement with observations. A cooling flow does exist in the moderate cooling flow model, but the mass cooling rate is P10% of that in old versions of cooling flow models.

show abstract

Bubbles in planetary nebulae and clusters of galaxies: Jet properties

Cited by 27 publications

References 44 publications

The evolution of M 2–9 from 2000 to 2010

The evolution of M 2–9 from 2000 to 2010

The formation of slow-massive-wide jets

Feedback Heating with Slow Jets in Cooling Flow Clusters

Contact Info

Product

Resources

About