Properties of the dust emission of the planetary nebula NGC 6445

Details Properties of the dust emission of the planetary nebula NGC 6445 Properties of the dust emission of the planetary nebula NGC 6445

Mar 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999esasp.427..417v&link_type=abstract

The Universe as Seen by ISO. Eds. P. Cox & M. F. Kessler. ESA-SP 427., p. 417

Computer Science

Planetary Nebulae

Scientific paper

In this paper we present new infrared spectra of the planetary nebula NGC 6445. These data show that the thermal emission from the grains is unusually cool and has a very low flux compared to Hβ. A model of the ionized region is constructed, using the photo-ionization code Cloudy 90.05. Based on this model we show from depletions in the gas phase elements that little grain destruction can have occurred in the ionized region of NGC 6445. We also find that there is no indication for dust-gas separation in the nebula. The most likely conclusion is that grains are residing inside the ionized region of NGC 6445 and that the low temperature and flux of the grain emission is caused by the low luminosity of the central star and the low optical depth of the grains. This implies that the grains in this nebula could survive exposure to hard UV photons for at least several thousands of years.

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