Hostname: page-component-78c5997874-ndw9j Total loading time: 0 Render date: 2024-11-17T19:40:00.588Z Has data issue: false hasContentIssue false
  • English
  • Français

On the Evolution of Proto-Planetary Nebulae

Published online by Cambridge University Press:  07 August 2017

J.Y. Hu ,
B.W. Jiang  and
S. Slijkhuis
J.Y. Hu
Affiliation:
Beijing Observatory, Academia Sinica, Beijing, 100080, China
B.W. Jiang
Affiliation:
Beijing Observatory, Academia Sinica, Beijing, 100080, China
S. Slijkhuis
Affiliation:
Astronomical Institute, University of Amsterdam, The Netherlands

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The ages of PNNe in our sample (Hu et al., 1990) were derived from the inner radius of the dust shell using the radiative transfer model fitting with SED and expansion velocities of envelopes obtained from radio molecular lines observations (if without radio data a Vexp of 15 km/sec was assumed). The objects are classified into the following groups:

  1. 1. invisible;

  2. 2. M-type;

  3. 3. F (or G)-type; and

  4. 4. F (or G)-type with Ra emission.

Type
IV. Planetary Nebulae Connection: Evolution from the AGB
Information
Symposium - International Astronomical Union , Volume 155: Planetary Nebulae , 1993 , pp. 337
Copyright
Copyright © Kluwer 1993 

References

Hu, J.Y., de Jong, T., Slijkhuis, S., 1990, ‘From Miras to Planetary Nebulae’, 487–489.Google Scholar
Slijkhuis, S., 1992, Ph.D. thesis, Chapter 6, Univ. of Amsterdam Google Scholar