Bubbles in planetary nebulae and clusters of galaxies: jet bending

Soker, Noam; Bisker, Gili

doi:10.1111/j.1365-2966.2006.10313.x

Cited by 19 publications

(23 citation statements)

References 57 publications

(95 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The morphologies of some PNe are observed to be similar to X-ray deficient bubbles in cooling flows (Soker & Bisker 2006), as presented in Figures 1 and 2, and to some nebulae around YSOs (e.g. Lee & Sahai 2004).…”

Section: Pn Morphologiesmentioning

confidence: 89%

The jet feedback mechanism (JFM) in stars, galaxies and clusters

Soker

2016

New Astronomy Reviews

149

106

View full text Add to dashboard Cite

I review the influence jets and the bubbles they inflate might have on their ambient gas as they operate through a negative jet feedback mechanism (JFM). I discuss astrophysical systems where jets are observed to influence the ambient gas, in many cases by inflating large, hot, and low-density bubbles, and systems where the operation of the JFM is still a theoretical suggestion. The first group includes cooling flows in galaxies and clusters of galaxies, star-forming galaxies, young stellar objects, and bipolar planetary nebulae. The second group includes core collapse supernovae, the common envelope evolution, the grazing envelope evolution, and intermediate luminosity optical transients. The suggestion that the JFM operates in these four types of systems is based on the assumption that jets are much more common than what is inferred from objects where they are directly observed. Common to all eight types of systems reviewed here is the presence of a compact object inside an extended ambient gas. The ambient gas serves as a potential reservoir of mass to be accreted on to the compact object. If the compact object launches jets as it accretes mass, the jets might reduce the accretion rate as they deposit energy to the ambient gas, or even remove the entire ambient gas, hence closing a negative feedback cycle.

show abstract

Section: Pn Morphologiesmentioning

confidence: 89%

The jet feedback mechanism (JFM) in stars, galaxies and clusters

Soker

2016

New Astronomy Reviews

149

106

View full text Add to dashboard Cite

show abstract

“…PSR , whereĖ jet is the jet power, R jet its radius, and ρ ISM is the medium mass density (see, e.g., Soker & Bisker 2006, and references therein), it follows that the jet has to be rather powerful and/or collimated. A high jet power is indeed supported by the relative distribution of the total X-ray luminosity of the system.…”

Section: Discussionmentioning

confidence: 99%

The long helical jet of the Lighthouse nebula, IGR J11014-6103

Pavan

Bordas

Puehlhofer

et al. 2014

A&A

View full text Add to dashboard Cite

Context. Jets from rotation-powered pulsars so far have only been observed in systems moving subsonically through their ambient medium and/or embedded in their progenitor supernova remnant (SNR). Supersonic runaway pulsars are also expected to produce jets, but they have not been confirmed so far. Aims. We investigated the nature of the jet-like structure associated with the INTEGRAL source IGR J11014-6103 (the "Lighthouse nebula"). The source is a neutron star escaping its parent SNR MSH 11-61A supersonically at a velocity exceeding 1000 km s −1 . Methods. We observed the Lighthouse nebula and its jet-like X-ray structure through dedicated high spatial resolution observations in X-rays (with Chandra) and in the radio band (with ATCA). Results. Our results show that the feature is a true pulsar's jet. It extends highly collimated over 11pc, displays a clear precessionlike modulation, and propagates nearly perpendicular to the system direction of motion, implying that the neutron star's spin axis in IGR J11014-6103 is almost perpendicular to the direction of the kick received during the supernova explosion. Conclusions. Our findings suggest that jets are common to rotation-powered pulsars, and demonstrate that supernovae can impart high kick velocities to misaligned spinning neutron stars, possibly through distinct, exotic, core-collapse mechanisms.

show abstract

“…Furthermore, the point-symmetric morphology of IC 4634, which gives the nebula its S-shaped appearance, and the varying sign of the radial velocity are commonly interpreted as being the direct result of a time-dependent direction of ejection of the source. In the next section, we explore in further detail this supposition, which may in general be of interest with regard to other point-symmetric PNe (Cliffe et al 1995;Lee & Sahai 2003;García-Arredondo & Frank 2004;Velázquez et al 2004;Soker & Bisker 2006).…”

Section: Observational Evidence and Similarities To Herbig-haro Objectsmentioning

confidence: 99%

Multiple and Precessing Collimated Outflows in the Planetary Nebula IC 4634

Guerrero

Miranda

Riera

et al. 2008

Astrophysical Journal

View full text Add to dashboard Cite

With its remarkable double-S shape, IC 4634 is an archetype of point-symmetric planetary nebulae ( PNe). In this paper, we present a detailed study of this PN using archival HST WFPC2 and ground-based narrowband images to investigate its morphology, and long-slit spectroscopic observations to determine its kinematics and to derive its physical conditions and excitation. The data reveal new structural components, including a distant string of knots distributed along an arclike feature 40 00 Y60 00 from the center of the nebula, a skin of enhanced [O iii]/ H ratio enveloping the inner shell and the double-S feature, and a triple-shell structure. The spatio-kinematical study also finds an equatorial component of the main nebula that is kinematically independent of the bright inner S-shaped arc. We have investigated in detail the bow shockYlike features in IC 4634 and found that their morphological, kinematical, and emission properties are consistent with the interaction of a collimated outflow with surrounding material. Indeed, the morphology and kinematics of some of these features can be interpreted using a three-dimensional numerical simulation of a collimated outflow precessing at a moderate, time-dependent velocity. Apparently, IC 4634 has experienced several episodes of point-symmetric ejections oriented in different directions, with the outer S-shaped feature being related to an earlier point-symmetric ejection, and the outermost arclike string of knots being the relic of a still much earlier point-symmetric ejection. There is tantalizing evidence that the action of these collimated outflows has also taken part in the shaping of the innermost shell and inner S-shaped arc of IC 4634. Subject headingg s: planetary nebulae: general -planetary nebulae: individual ( IC 4634) -stars: winds, outflows

show abstract

Bubbles in planetary nebulae and clusters of galaxies: jet bending

Cited by 19 publications

References 57 publications

The jet feedback mechanism (JFM) in stars, galaxies and clusters

The jet feedback mechanism (JFM) in stars, galaxies and clusters

The long helical jet of the Lighthouse nebula, IGR J11014-6103

Multiple and Precessing Collimated Outflows in the Planetary Nebula IC 4634

Contact Info

Product

Resources

About