Polycyclic Aromatic Hydrocarbon Formation in O-rich Planetary Nebulae

By Keith Cowing
March 16, 2014
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Polycyclic Aromatic Hydrocarbon Formation in O-rich Planetary Nebulae

Polycyclic aromatic hydrocarbons (PAHs) have been observed in O-rich planetary nebulae towards the Galactic Bulge.

This combination of oxygen-rich and carbon-rich material, known as dual-dust or mixed chemistry, is not expected to be seen around such objects. We recently proposed that PAHs could be formed from the photodissociation of CO in dense tori. In this work, using VISIR/VLT, we spatially resolved the emission of the PAH bands and ionised emission from the [SIV] line, confirming the presence of dense central tori in all the observed O-rich objects.

Furthermore, we show that for most of the objects, PAHs are located at the outer edge of these dense/compact tori, while the ionised material is mostly present in the inner parts of these tori, consistent with our hypothesis for the formation of PAHs in these systems. The presence of a dense torus has been strongly associated with the action of a central binary star and, as such, the rich chemistry seen in these regions may also be related to the formation of exoplanets in post-common-envelope binary systems.

L. Guzman-Ramirez, E. Lagadec, D. Jones, A. A. Zijlstra, K. Gesicki (Submitted on 7 Mar 2014)

Comments: 14, accepted for publication in the MNRAS Journal

Subjects: Solar and Stellar Astrophysics (astro-ph.SR)

Cite as: arXiv:1403.1856 [astro-ph.SR (or arXiv:1403.1856v1 [astro-ph.SR] for this version) Submission history

From: Lizette Guzman-Ramirez PhD [v1] Fri, 7 Mar 2014 19:47:49 GMT (10402kb,D)

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