The evolution of asymptotic giant branch stars in the Large Magellanic Cloud

Details The evolution of asymptotic giant branch stars in the Large Magellanic Cloud The evolution of asymptotic giant branch stars in the Large Magellanic Cloud

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...284...98r&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 284, Sept. 1, 1984, p. 98-107. Research supported by the Science and Engine

Mathematics

66

Asymptotic Giant Branch Stars, Functions (Mathematics), Giant Stars, Magellanic Clouds, Stellar Evolution, Stellar Luminosity, B Stars, Cepheid Variables, Cosmos Satellites, Infrared Spectra, Mass To Light Ratios, Stellar Mass Ejection, Stellar Spectrophotometry, Visible Spectrum

Scientific paper

A bolometric luminosity function is presented for stars on the asymptotic giant branch (AGB) in a 15 deg sq area of the Large Magellanic Cloud (LMC). The luminosity function was derived by COSMOS scanning of multiple visual and infrared UK Schmidt plates and is photometrically complete for V - I greater than 1.6. The deficiency of luminous AGB stars which was apparent in earlier spectroscopic studies is seen in this study also. This rules out the notion that the deficiency is due to nuclear processing of carbon-rich envelopes to spectroscopically normal composition. A more likely explanation is that mass loss more severe than is predicted by standard scaling relations sets in on the upper AGB, terminating the evolution of these stars at quite modest luminosities. Significant variations in the AGB luminosity function are seen over the field. These are best understood as a consequence of different star formation histories in different locations in the LMC.

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