Masers Diagnostics to Identify Stars Departing from the AGB

Details Masers Diagnostics to Identify Stars Departing from the AGB Masers Diagnostics to Identify Stars Departing from the AGB

Aug 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001assl..265..417e&link_type=abstract

Post-AGB Objects as a Phase of Stellar Evolution, Proceedings of the Toruń Workshop held July 5-7, 2000. Edited by R. Szczerba a

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

In a number of Proto-Planetary Nebulae (PPN) candidates maser emission has been found, most often from OH. Their properties are distinctively different from those in AGB stars, reflecting the change from a radially symmetric mass-loss process on the Asymptotic Giant Branch to other mostly axisymmetric geometries. Interferometric maps indicate that during the PPN stage, when a bipolar morphology develops, the OH masers are located in radial outflows associated with the equatorial disc. H2O masers can be associated with the dying superwind or with the newly developing bipolar outflows. SiO masers are rarely detected. Peculiar maser properties of IRAS sources with infrared colors similar to Mira variables and OH/IR stars can be used to pinpoint PPN in the making.

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