POLYCYCLIC AROMATIC HYDROCARBON EMISSION IN THE PROPLYD HST10: WHAT IS THE MECHANISM BEHIND PHOTOEVAPORATION?

@article{Vicente2013POLYCYCLICAH,
  title={POLYCYCLIC AROMATIC HYDROCARBON EMISSION IN THE PROPLYD HST10: WHAT IS THE MECHANISM BEHIND PHOTOEVAPORATION?},
  author={S{\'i}lvia Vicente and O. Bern{\'e} and A. Tielens and Nuria Huelamo and E. E. Pantin and Inga Kamp and Andres Carmona},
  journal={The Astrophysical Journal Letters},
  year={2013},
  volume={765}
}
Proplyds are photodissociation-region-(PDR)-like cometary cocoons around young stars which are thought to originate through photoevaporation of the central protoplanetary disk by external UV radiation from the nearby OB stars. This Letter presents spatially resolved mid-infrared imaging and spectroscopy of the proplyd HST10 obtained with the Very Large Telescope/VISIR instrument. These observations allow us to detect polycyclic aromatic hydrocarbon (PAH) emission in the proplyd PDR and to study… 
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References

SHOWING 1-10 OF 29 REFERENCES
Spatially extended polycyclic aromatic hydrocarbons in circumstellar disks around T Tauri and Herbig Ae stars
Aims. Our aim is to determine the presence and location of the emission from polycyclic aromatic hydrocarbons (PAHs) towards low and intermediate mass young stars with disks using large aperture
Photodissociation Region Models of Photoevaporating Circumstellar Disks and Application to the Proplyds in Orion
We have modeled the neutral flows emerging from circumstellar disks or small clumps of size r0 illuminated by an external source of ultraviolet radiation. The models are applied to the disks
MOLECULAR LINE EMISSION FROM A PROTOPLANETARY DISK IRRADIATED EXTERNALLY BY A NEARBY MASSIVE STAR
Star formation often occurs within or nearby stellar clusters. Irradiation by nearby massive stars can photoevaporate protoplanetary disks around young stars (so-called proplyds) which raises
Disks, Microjets, Windblown Bubbles, and Outflows in the Orion Nebula
New deep narrowband images of the Orion Nebula obtained with WFPC2 on the Hubble Space Telescope (HST) and spectra taken with the HIRES spectrometer at the Keck Observatory are presented. We report
Nonequilibrium Photodissociation Regions with Advancing Ionization Fronts
We have modeled the thermal and chemical structure of photodissociation regions (PDRs) where the interface between the H II region and the neutral cloud (the ionization front IF) is moving with a
Formation of buckminsterfullerene (C60) in interstellar space
TLDR
It is argued that polycyclic aromatic hydrocarbons are converted into graphene, and subsequently C60, under UV irradiation from massive stars, shows that alternative—top-down—routes are key to understanding the organic inventory in space.
Photoevaporation of Disks and Clumps by Nearby Massive Stars: Application to Disk Destruction in the Orion Nebula
We present a model for the photoevaporation of circumstellar disks or dense clumps of gas by an external source of ultraviolet radiation. Our model includes the thermal and dynamic effects of 6-13.6
3D numerical simulations of photodissociated and photoionized disks
Aims. In this work we study the influence of the UV radiation field of a massive star on the evolution of a disklike mass of gas and dust around a nearby star. This system has similarities with the
2.12 Micron Molecular Hydrogen Emission from Circumstellar Disks Embedded in the Orion Nebula
We present narrowband images of two externally illuminated circumstellar disks embedded in the Orion Nebula. The images were taken with camera 2 of the Near-Infrared Camera and Multiobject
A Keck High-Resolution Spectroscopic Study of the Orion Nebula Proplyds
We present the results of spectroscopy of four bright proplyds in the Orion Nebula obtained at a velocity resolution of 6 km s-1. After careful isolation of the proplyd spectra from the confusing
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