The occurrence of carbon stars and Cepheid variables in common fields of the Magellanic Clouds

Details The occurrence of carbon stars and Cepheid variables in common fields of the Magellanic Clouds The occurrence of carbon stars and Cepheid variables in common fields of the Magellanic Clouds

Sep 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...260..695b&link_type=abstract

Astrophysical Journal, Part 1, vol. 260, Sept. 15, 1982, p. 695-706.

Astronomy and Astrophysics

Astrophysics

10

Carbon Stars, Cepheid Variables, Magellanic Clouds, Stellar Evolution, Stellar Luminosity, Asymptotic Giant Branch Stars, Giant Stars, Nuclear Fusion, Stellar Envelopes, Stellar Mass, Stellar Structure, Tables (Data)

Scientific paper

It has been suggested that the apparent lack of carbon stars brighter than M(bol) = -6.5 in the Magellanic Clouds may be due to an 'age effect' in the fields that have been studied. This 'age effect' implies that no recent star formation has occurred and that consequently the individual mass of any of the remaining stars is too small to produce very bright carbon stars. To test this hypothesis, these same fields are searched for Cepheid variables whose presence would on the contrary indicate that recent star formation has taken place. It is found that Cepheids occur in nearly all of the studied fields, which invalidates the 'age effect' hypothesis. It is argued that carbon stars are not observed brighter than M(bol) = -6.5 because of the effect of 'envelope burning' following the dredge-up episodes. Instead, asymptotic giant branch stars having luminosities with M(bol) between -6.5 and -7.3 should be seen as 'red variables,' bright early M giants, or possibly early M supergiants.

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