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Dynamical Structures of Planetary Nebulae — Models Against Observations

Published online by Cambridge University Press:  07 August 2017

H. Marten ,
K. Gesicki  and
R. Szczerba
H. Marten
Affiliation:
1Institut für Theoretische Physik und Sternwarte der Universität Kiel Olshausenstr. 40, D-2300 Kiel, Germany
K. Gesicki
Affiliation:
2Copernicus Astronomical Center, Laboratory of Astrophysics ul. Chopina 12/18, 87-100 Toruń, Poland
R. Szczerba
Affiliation:
2Copernicus Astronomical Center, Laboratory of Astrophysics ul. Chopina 12/18, 87-100 Toruń, Poland

Abstract

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Hydrodynamical calculations of Planetary Nebulae (PNe) over 25000 yrs of evolution which include timedependent effects of ionization as well as variable central stars winds and parameters consistent with stellar model calculations show a great variety of velocity and density structures which strongly deviate from the often assumed “homogeneous shells, expanding with constant velocities” (Marten & Schönberner, 1991, hereafter MS). By means of a static photoionization code we calculate the surface brightness in the 10 most prominent nebular emission lines for density structures of the model sequence “VS” as given by MS. The obtained radial emissivities are used together with the velocity and temperature structure of the ionized gas to calculate (thermally broadened) line profiles in order to derive “measured” expansion velocities. We compare the theoretical surface brightnesses with observations and demonstrate some difficulties in the interpretation of nebular expansion velocities, expansion distances and ages.

Type
IV. Planetary Nebulae Connection: Evolution from the AGB
Information
Symposium - International Astronomical Union , Volume 155: Planetary Nebulae , 1993 , pp. 315 - 318
Copyright
Copyright © Kluwer 1993 

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