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Figure 1:
Top: evolutionary path for the
0.595
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Figure 2: Initial model used in this paper. Plotted are the density of the heavy particles (thick), of the electrons (dotted), and the flow velocity (thin) against the distance from the central star. |
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Figure 3:
Heavy-particle density (thick), electron density
(dotted), and velocity field (thin) together with the
[O III] and [N II] surface brightnesses and emission-line
profiles of hydrodynamical models at selected positions along the
horizontal part of the 0.595 ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 4:
Detailed illustration of how the kinematical properties of our model PN
from Fig. 3 develop with time while the central star
evolves across the HR diagram as shown in Fig. 1.
Material velocities are indicated by V, motions of structures by
![]() Top, left: for the shell, the velocities (in the stellar rest frame) of the shock front, ![]() ![]() Top, right: corresponding velocities for the rim, except that instead of the post-shock velocity we plotted its pre-shock velocity, ![]() ![]() Middle: mach numbers of the resp. shocks, ![]() ![]() ![]() Bottom: kinematic ages, ![]() |
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Figure 5:
Radial displacements of shell, rim and contact surface of a model PN
as a function of time. Plotted are
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Figure 6:
Comparison of different kinematical ages derived from the shell radius.
They are computed from our hydrodynamical models and plotted as a
function of their real evolutionary age. The curves for
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Figure 7:
Top:
normalized surface brightness distributions in [O III] of three
selected planetary nebulae from HST monochromatic images (F502N),
with effective temperatures of their central stars increasing
from left to right (cf. Table 1). For NGC 3242
the He II image (F469N) is added.
The cuts are taken along or close to the minor axes and
scaled to the model sizes.
Bottom:
normalized surface-brightness distributions in [O III]
5007 Å (and additionally in He II 4686 Å in the case of
NGC 3242) for selected hydrodynamical models that match
the observations as closely as possible.
The positions of the models along the track shown in
Fig. 1 are ( from left to right) at
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Figure 8: Spectroscopic expansion velocities of the objects from Table 1 compared with predictions from the models used in Fig. 7. The dashed line is the 1:1 relation. |
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Figure 9:
Top:
radial H![]() ![]() ![]() ![]() ![]() |
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Figure 10:
Kinematic expansion time scales,
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Figure 11:
Detailed illustration of the different possible correction
factors
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Figure 12:
Same as in Fig. 11, but now for hydrodynamical models
with a central star of 0.696 ![]() |
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Figure A.1:
Same as in Fig. 1 but for a 0.696 ![]() |
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Figure A.2:
Same as in Fig. 3 but for a 0.696 ![]() ![]() ![]() ![]() ![]() |
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Figure A.3:
Same as in Fig. 4 but now for the sequence
with the 0.696 ![]() |
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Figure A.4:
Same as in Fig. 5 but now for the sequence
with the 0.696 ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() |