Models of planetary nebulae with dust

Details Models of planetary nebulae with dust Models of planetary nebulae with dust

Nov 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...202..195f&link_type=abstract

Astrophysical Journal, vol. 202, Nov. 15, 1975, pt. 1, p. 195-203.

Astronomy and Astrophysics

Astrophysics

55

Astronomical Models, Computerized Simulation, Cosmic Dust, Interstellar Matter, Planetary Nebulae, Infrared Spectra, Interstellar Gas, Mathematical Models, Pressure Effects, Radiative Heat Transfer, Stellar Radiation

Scientific paper

Computer models have been constructed of planetary nebulae of 0.15 and 0.5 solar mass, containing varying amounts of absorbing dust grains. In all cases the dust remained well mixed with the gas, and was responsible for the maintenance of a well-defined inner edge for the nebular shell. Once the nebula was ionized, the expansion in the outer regions accelerated due to pressure gradients, so that the observed mass decreased with time. The more massive nebulae were found to expand more slowly. Even when all of the L-alpha radiation was absorbed by grains, it was not as important for grain heating and acceleration as the direct stellar radiation. Agreement with several aspects of recent infrared observations was obtained.

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