Photofission production of technetium and synthetic asymptotic giant branch evolution

Details Photofission production of technetium and synthetic asymptotic giant branch evolution Photofission production of technetium and synthetic asymptotic giant branch evolution

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...347..989l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 347, Dec. 15, 1989, p. 989-997.

Astronomy and Astrophysics

Astrophysics

16

Asymptotic Giant Branch Stars, Cosmochemistry, Mira Variables, Nuclear Fission, Stellar Evolution, Technetium, Nuclear Fusion, Stellar Atmospheres, Stellar Interiors, Stellar Models, Zirconium

Scientific paper

Synthetic asymptotic giant branch (AGB) evolution calculations are carried out in order to investigate further the recent suggestion that detectable quantities of technetium could be produced in the atmospheres of AGB stars following the photofission of any actinide isotopes initially present. It is found that any technetium so produced can only become detectable when the envelope mass is reduced below about 0.2 solar mass which corresponds to the final stage of the star's evolution on the AGB. It is estimated that stars with masses (at the first thermal pulse) in the range 1-2 solar masses are most likely to give rise to a detectable technetium abundance when values of Mbol between -4.5 and -6 are reached. It is noted that this coincides with the Mira phase of evolution, where most of the stellar technetium detections are made. Although some quantitative differences between this photofission production theory and observation may exist, it is argued that more serious difficulties are associated with an s-process production mechanism for technetium.

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