Statistics – Computation
Scientific paper
Dec 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...347..307b&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 347, Dec. 1, 1989, p. 307-324. Research supported by the Computer Sciences
Statistics
Computation
19
Computational Astrophysics, Hydrodynamics, Planetary Nebulae, Stellar Evolution, Stellar Models, Emission Spectra, Hydrogen, Photoionization, Red Giant Stars, Stellar Temperature, Ultraviolet Radiation
Scientific paper
Numerical models of PN have been calculated using the equations of mass, momentum, and energy conservation. Theoretical arguments and calculations indicated that the turn-on time scale for UV radiation is 100-1000 yr. In the standard model, the initial inner radius of the gaseous shell is 7 x 10 to the 16th cm and the initial outer radius is 1 x 10 to the 17th cm. The initial density distribution is proportional to 1/r-squared, and the central star increases in temperature from 10,000 to 50,000 K in 100 yr with a constant luminosity of 10,000 solar. Six other models are presented, each of which differs from the standard model in only one parameter. All models have a uniform initial velocity of 30 km/s. UV photons from the central star produce an ionization front which progresses through the nebular gas. The dynamical effects of the stellar turn-on are calculated as the front moves through the nebula and alters its physical conditions.
Bobrowsky Matthew
Zipoy David M.
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