First ISO Results on the 'Born-Again' Object A78

Details First ISO Results on the 'Born-Again' Object A78 First ISO Results on the 'Born-Again' Object A78

May 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999iso..work..105g&link_type=abstract

Proceedings of 2nd Austrian ISO Conference, Vienna May 1999, eds. Hron, J.; Hoefner, S.

Physics

Planetary Nebulae, Iso

Scientific paper

The planetary nebula A78 (PN G081.2-14.9) belongs to a small group of objects (including e.g. Sakurai's Object, A30, A58, NGC650-51) which are characterized by hydrogen-deficient dusty ejecta producing strong thermal IR emission. This ejecta has been found to have a high dust/gas ratio (Borkowski et al. 1994). These objects are supposed to have undergone a late He-flash (Iben et al. 1983 and 1984) and are suspected to be connected to the PG1159-035 type central stars of planetary nebulae (CSPN). The ignition of the remnant He-shell not only sends them back into the AGB region of the HRD (thus 'born-again' objects), as they retrace the post-AGB evolution towards higher surface temperatures a second PN phase occurs with a timescale 3 times longer than that of the initial hydrogen-burning phase (Iben et al. 1991). Assuming that the same mass loss mechanism that has expelled the hydrogen-rich envelope during the first post-AGB track is at work in this second phase again, a strong wind will eject highly processed, hydrogen-poor material.

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