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Spherically Symmetric Kinematic Modelling of Planetary Nebulae

Published online by Cambridge University Press:  07 August 2017

C. Diesch  and
M. Grewing
C. Diesch
Affiliation:
(1)Astronomisches Institut der Universität Waldhäuserstraße 64, D-7400 Tübingen
M. Grewing
Affiliation:
(1)Astronomisches Institut der Universität Waldhäuserstraße 64, D-7400 Tübingen (2)Institute for Radioastronomy at Millimeter Wavelengths (IRAM) 300, rue de la Piscine, Domaine Universitaire, F-38406 St. Martin d'Hères, France

Abstract

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High resolution two-dimensional long slit spectra of NGC 7009, NGC 3242, IC 2448 and TC 1 in the Hα(6565 Å), OIII(5007 Å) and NII(6584 Å) emission lines have been used as input to determine radial velocity gradients in PNe by fitting calculated high resolution spatially resolved spectral structures of single emission lines. Contributions to the Doppler structure of emission lines taken into account are the global expansion of the PN shell and thermal line broadening due to temperatures of some 104 K. This model is based on two parametrized empirically chosen spherical symmetric functions:

  1. 1. A empirical two parameter density function ρ(r).

  2. 2. A linear radial velocity component function ν(r).

Type
IV. Planetary Nebulae Connection: Evolution from the AGB
Information
Symposium - International Astronomical Union , Volume 155: Planetary Nebulae , 1993 , pp. 374
Copyright
Copyright © Kluwer 1993 

References

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