UV-NIR spectra of two planetary nebulae with X-Shooter

Szyszka, C.; Walsh, J. R.; Zijlstra, A. A.

doi:10.1017/s1743921312012161

Cited by 8 publications

(10 citation statements)

References 4 publications

(7 reference statements)

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“…Many new observations and theoretical studies since the turn of the Millennium further consolidated the jet-shaping scenario of many PNe (e.g., Parthasarathy et al 2000;Bujarrabal et al 2001;Miranda et al 2001;Corradi et al 2001b;Guerrero et al 2001;Imai et al 2002;Riera et al 2003;Vinković et al 2004;Huggins et al 2004;Peña et al 2004;Balick & Hajian 2004;Arrieta et al 2005;Oppenheimer et al 2005;Sahai et al 2005;Vlemmings et al 2006;Miranda et al 2010;Nakashima et al 2010;Phillips et al 2010;Sahai et al 2011;Szyszka et al 2011;López et al 2012;Clark et al 2013;Pérez-Sánchez et al 2013;Vlemmings et al 2014;Fang et al 2015 Dennis et al 2008Dennis et al , 2009Lee et al 2009;Huarte-Espinosa et al 2012;Velázquez et al 2012;Balick et al 2013;Velázquez et al 2014 for theoretical studies; these papers composed a small fraction of the papers studying jets in PNe). X-ray observations seem also to support the presence of jet-inflated bubbles and of jets Sahai et al 2003), similar to X-ray jets in symbiotic systems (e.g., Kellogg et al 2001;Galloway & Sokoloski 2004).…”

Section: Pn Morphologiesmentioning

confidence: 99%

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

Soker

2016

New Astronomy Reviews

149

106

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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.

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Section: Pn Morphologiesmentioning

confidence: 99%

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

Soker

2016

New Astronomy Reviews

149

106

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“…This complicated structure might come from a triple-stellar evolution. NGC 6302 (PN G349.5+01.0) (e.g., Meaburn et al 2005;Szyszka et al 2011). It has a well define bipolar structure, but with another pair of lobes protruding from the main bipolar structure.…”

Section: The Descendant Pnementioning

confidence: 99%

Planetary nebula progenitors that swallow binary systems

Soker

2015

Monthly Notices of the Royal Astronomical Society

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I propose that some irregular 'messy' planetary nebulae owe their morphologies to triple-stellar evolution where tight binary systems evolve inside and/or on the outskirts the envelope of asymptotic giant branch (AGB) stars. In some cases the tight binary system can survive, in other it is destroyed. The tight binary system might breakup with one star leaving the system. In an alternative evolution, one of the stars of the brook-up tight binary system falls toward the AGB envelope with low specific angular momentum, and drowns in the envelope. In a different type of destruction process the drag inside the AGB envelope causes the tight binary system to merge. This releases gravitational energy within the AGB envelope, leading to a very asymmetrical envelope ejection, with an irregular and 'messy' planetary nebula as a descendant. The evolution of the triple-stellar system can be in a full common envelope evolution (CEE) or in a grazing envelope evolution (GEE). Both before and after destruction (if take place) the system might lunch pairs of opposite jets. One pronounced signature of triple-stellar evolution might be a large departure from axisymmetrical morphology of the descendant planetary nebula. I estimate that about one in eight non-spherical PNe is shaped by one of these triple-stellar evolutionary routes.

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“…7). The lobes and the innermost parts of the nebula are expanding with a velocity increasing with the radial distance (Szyszka et al 2011). At the center, there is a high extinction molecular torus, oriented north-south, roughly perpendicular to the axis of the lobes, and expanding slowly with a velocity of 8 km s −1 (Peretto et al 2007).…”

Section: Introductionmentioning

confidence: 99%

Spectroscopic mapping of the planetary nebula NGC 6302

Rauber

Copetti

Krabbe

2014

A&A

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Context. Most spectroscopic studies of planetary nebulae (PNe) are based on data from specific parts of the objects. Considering the high complexity of their morphological structures, integrated or average values across an observed region can only provide limited information of their ionic, density, and temperature structures. Aims. We investigate the spatial variation of the physical and chemical properties of NGC 6302, a high-ionization PNe, with a complex bipolar structure. Methods. Spatially resolved long-slit spectroscopic data were obtained from 11 parallel and equally spaced directions over the nebula. Integrated spectra were also obtained and 142 lines were identified. Results. The electron density maps show a peaked distribution, with the densest area at the circumstellar region, reaching N e ≈ 40 000 cm −3 , and decreasing to N e ≤ 1000 cm −3 at the lobes. Knots were observed in the N e (S ii) map, with 2000 cm −3 < N e < 3000 cm −3 . The N e (Ar iv) map suggests the presence of an inner region with N e ≈ 20 000 cm −3 that extends from the center through the east lobe. A homogeneous temperature distribution was found for both T e (O iii) and T e (N ii). Small temperature fluctuations on the plane of the sky of t 2 s (N ii) = 0.0071 and t 2 s (O iii) = 0.0043 were estimated.Conclusions. In general, the total abundances obtained are similar to the maximum found in the ionic abundance maps of the dominant ionic species. This demonstrates the potential of spatially resolved abundance studies for establishing lower limits of the total abundances based on ionic abundances, for checking the ionization correlation factors, and in some cases, for determining the total abundances directly from maps of ionic abundances.

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UV-NIR spectra of two planetary nebulae with X-Shooter

Cited by 8 publications

References 4 publications

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

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

Planetary nebula progenitors that swallow binary systems

Spectroscopic mapping of the planetary nebula NGC 6302

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