Planetary and Proto-Planetary Nebulae: From IRAS to ISO: Proceedings of the Frascati Workshop 1986, Vulcano Island, September 812, 1986 [Paperback]

There are two questions that we can ask ourselves in order to describe this workshop. The first question is a double question: why a conference on this subject and why a workshop? The first idea of organizing this workshop came while reading the scientific objectives of one of the instruments onboard the ISO satel? lite (a phase A document concerning the IR camera). On going through the scientific motivations for building the instrument I realized with surprise that no mention was made of Planetary Nebulae (PN). At present this is no longer true. There is a chapter indicating the capabilities of the camera in the PN field and what we can reasonably expect from that instrument. But it was at this moment that the first idea of organizing a workshop on the subject of PN came. Of course there are other, stronger motivations. The first one is that I think this is the right moment after IRAS. I think we all spent the last two or three years working on IRAS data. IRAS represented a corner-stone for those working on Planetary Nebulae: the amount of data that came out of the instruments onboard the satellite was enormous and opened up new ways of looking at planetary nebulae, as well as at other fields.Session I..- Infrared emission from young planetary nebulae.- Advances in knowledge of planetary nebulae from UV astronomy.- Status of the spectroscopic survey of planetary nebulae.- Session II..- Announcement  The Strasbourg-ESO Catalogue of galactic planetary nebulae.- IRAS Additional Observations of planetary nebulae.- Spectroscopy at 813pm as a probe of the carbon to oxygen ratio in planetary nebulae.- Session III..- Protoplanetary nebulae.- The evolution from Miras to planetary nebulae as derived from observations of Miras and OH/IR stars.- The position of PN nuclei in the H-R diagram: present status.- On the nitrogen and helium enrichment of the interstellar medium.- Temperatures, luminosities and mass loss rates for PN nuclei.- An outflow model for bipolar planetarylCa