A silicate dust model for the halo planetary DDDM-1

Details A silicate dust model for the halo planetary DDDM-1 A silicate dust model for the halo planetary DDDM-1

Dec 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988mnras.235.1049h&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 235, Dec. 15, 1988, p. 1049-1058. Research supported by

Astronomy and Astrophysics

Astronomy

11

Infrared Astronomy Satellite, Planetary Nebulae, Silicates, Photoionization, Temperature Distribution, Thermal Emission

Scientific paper

A combined photoionization and dust model is presented for the carbon-poor, optically thick, planetary nebula in the galactic halo, DDDM-1. The abundance of silicate grains is varied to produce a match with observed IRAS fluxes at 25 and 60 μm. The derived dust-to-gas ratio, 1.1×10-3, is about a factor 5 lower than the ratio for disc planetaries of similar size. Details are given of the heating and temperature distribution of grains in this type of planetary nebula with a neutral region. Upper limits for the infrared fluxes of two other galactic halo nebulae are given. It is suggested that DDDM-1 is the only such object detected because of its higher abundance of heavy elements.

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