A spatio-kinematic model for the multiple shell planetary nebula NGC 1535

Details A spatio-kinematic model for the multiple shell planetary nebula NGC 1535 A spatio-kinematic model for the multiple shell planetary nebula NGC 1535

Oct 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...250..165b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 250, no. 1, Oct. 1991, p. 165-170. Research supported by Department of Space a

Astronomy and Astrophysics

Astrophysics

2

Planetary Nebulae, Shell Stars, Stellar Models, Dynamic Models, Emission Spectra, Fabry-Perot Spectrometers, Line Spectra

Scientific paper

High-resolution, Fabry-Perot observations are presented at selected positions of the multiple-shell planetary nebula NGC 1535 in the (O III) 5007 A line. Emission-line profiles are constructed based on a spatio-kinematic model for the nebula and are compared with the observations. It is seen that the kinematics of NGC 1535 may be explained by assuming the inner shell to be of a spherical form but constricted by a torus of dense material. The observed line profiles indicate that the physical conditions in the nebula may be explained by a model which is based on the assumptions of a constant expansion velocity in the (O III) line emitting region of 21 km/s for the inner shell, an nc(r) varies as r exp -3 relationship for the dependence of electron density on distance and the presence of turbulence in the main shell having a most probable velocity of 7.5 km/s. There is confirming evidence that the faint, outer shell of NGC 1535 is spheroidal in form.

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