An Asymmetric Jet-Launching Model for the Protoplanetary Nebula CRL 618

Velázquez, P. F.; Riera, A.; Raga, A. C.; Toledo-Roy, J. C.

doi:10.1088/0004-637x/794/2/128

Cited by 22 publications

(22 citation statements)

References 41 publications

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“…Here, we are considering the case of binarity. In fact, it has been suggested that the morphological structures of CRL 618 and IRC +10216, two well-studied evolved stars, are due to binary companions (Velázquez et al 2014;Cernicharo et al 2015). The numerical simulations of de Val-Borro et al (2009) of mass accretion of wind onto an AGB companion suggest this scenario is reasonable.…”

Section: Ions In the Circumstellar Envelope Of Agb Starsmentioning

confidence: 99%

“…However, more observations are necessary to constrain the intensity and periodicity of these events in T Dra and other AGB stars, as well as the role in its inner shell. Nevertheless, the presence of a companion star should not be considered surprising, since it has been proposed for well-studied evolved stars, such as IRC +10216 and the pre-planetary nebula CRL 618 (Velázquez et al 2014;Cernicharo et al 2015;Kim et al 2015). …”

Section: Introductionmentioning

confidence: 99%

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Single and Double Photoionization and Photodissociation of Toluene by Soft X-Rays in a Circumstellar Environment

Monfredini¹,

Fantuzzi²,

Nascimento³

et al. 2016

ApJ

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The formation of polycyclic aromatic hydrocarbons (PAHs) and their methyl derivatives mainly occurs in the dust shells of asymptotic giant branch (AGB) stars. The bands at 3.3 and 3.4 μm, observed in infrared emission spectra of several objects, are attributed C-H vibrational modes in aromatic and aliphatic structures, respectively. In general, the feature at 3.3 μm is more intense than that at 3.4 μm. Photoionization and photodissociation processes of toluene, the precursor of methylated PAHs, were studied using synchrotron radiation at soft X-ray energies around the carbon K edge using time-of-flight mass spectrometry. Partial ion yields of a large number of ionic fragments were extracted from single and 2D-spectra, where electron-ion coincidences have revealed the doubly charged parent molecule and several doubly charged fragments containing seven carbon atoms with considerable abundance. Ab initio calculations based on density functional theory were performed in order to elucidate the chemical structure of these stable dicationic species. The survival of the dications subjected to hard inner shell ionization suggests that they could be observed in the interstellar medium, especially in regions where PAHs are detected. The ionization and destruction of toluene induced by X-rays were examined in the T Dra conditions, a carbon-rich AGB star. In this context, a minimum photodissociation radius and the half-life of toluene subjected to the incidence of the soft X-ray flux emitted from a companion white dwarf star were determined.

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Section: Ions In the Circumstellar Envelope Of Agb Starsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Single and Double Photoionization and Photodissociation of Toluene by Soft X-Rays in a Circumstellar Environment

Monfredini¹,

Fantuzzi²,

Nascimento³

et al. 2016

ApJ

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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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“…Bipolar nebulae around evolved stars, such as planetary nebulae (PNe), are thought by many researchers to be shaped by jets that inflate bubbles inside a dense wind, (e.g, Morris 1987;Corradi & Schwarz 1993;Sahai & Trauger 1998;García-Segura et al 2005;Soker 2007;García-Díaz et al 2008;Akashi & Soker 2008a;Dennis et al 2008Dennis et al , 2009Lee et al 2009;Velázquez et al 2011;Boffin et al 2012;Huarte-Espinosa et al 2012;Akashi & Soker 2013;Balick et al 2013;Thomas et al 2013;Riera et al 2014;Tocknell et al 2014;Velázquez et al 2014;Zijlstra 2015). These bubbles can lead to other morphological features such as a dense equatorial outflow (Soker & Rappaport 2000;Akashi & Soker 2008b;Akashi et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Bipolar rings from jet-inflated bubbles around evolved binary stars

Akashi¹,

Soker²

2016

Mon. Not. R. Astron. Soc.

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We show that a fast wind that expands into a bipolar nebula composed of two opposite jetinflated bubbles can form a pair of bipolar rings around giant stars. Our model assumes three mass loss episodes: a spherical slow and dense shell, two opposite jets, and a spherical fast wind. We use the FLASH hydrodynamical code in three-dimensions to simulate the flow, and obtain the structure of the nebula. We assume that the jets are launched from an accretion disk around a stellar companion to the giant star. The accretion disk is assumed to be formed when the primary giant star and the secondary star suffer a strong interaction accompanied by a rapid mass transfer process from the primary to the secondary star, mainly a main sequence star. Later in the evolution the primary star is assumed to shrink and blow a fast tenuous wind that interacts with the dense gas on the surface of the bipolar structure. We assume that the dense mass loss episode before the jets are launched is spherically symmetric. Our results might be applicable to some planetary nebulae, and further emphasize the large variety of morphological features that can be formed by jets. But we could not reproduce some of the properties of the outer rings of SN 1987A. It seems that some objects, like SN 1987A, require a pre-jets mass loss episode with a mass concentration at mid-latitudes.

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An Asymmetric Jet-Launching Model for the Protoplanetary Nebula CRL 618

Cited by 22 publications

References 41 publications

Single and Double Photoionization and Photodissociation of Toluene by Soft X-Rays in a Circumstellar Environment

Single and Double Photoionization and Photodissociation of Toluene by Soft X-Rays in a Circumstellar Environment

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

Bipolar rings from jet-inflated bubbles around evolved binary stars

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