EVANS, A; RAWLINGS, JMC; (1994) PAH EMISSION IN NOVAE. MON NOT R ASTRON SOC , 269 (2) 427 - 434.
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We consider the origin of the 'PAH' emission reported in recent novae. We show that free PAH molecules would not survive in the environment of a nova and that the 'PAH' emission is more likely to have arisen in hydrogenated amorphous carbon (HAC) grains, which probably rehydrogenate after the dust has dispersed; we predict the appearance of extended red emission at this time. Furthermore, since the infrared properties of nitrogenated carbon are significantly different from those of hydrogenated carbon in the 6-8 mum range and novae are normally overabundant in nitrogen, carbon dust grains originating in novae are likely to be uniquely identifiable as such.
|Title:||PAH EMISSION IN NOVAE|
|Keywords:||MOLECULAR PROCESSES, CIRCUMSTELLAR MATTER, NOVAE, CATACLYSMIC VARIABLES, DUST, EXTINCTION, INFRARED, GENERAL, INFRARED, STARS, EXTENDED RED EMISSION, UNIDENTIFIED INFRARED-EMISSION, CARBON GRAINS, INTERSTELLAR, DUST, MOLECULES, DESTRUCTION, FULLERANES, CHEMISTRY, NEBULAE|
|UCL classification:||UCL > School of BEAMS > Faculty of Maths and Physical Sciences > Physics and Astronomy|
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