Pulsational Evidence for Mass Loss in NGC 1866 Cepheids

Details Pulsational Evidence for Mass Loss in NGC 1866 Cepheids Pulsational Evidence for Mass Loss in NGC 1866 Cepheids

Oct 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aj....128.1597b&link_type=abstract

The Astronomical Journal, Volume 128, Issue 4, pp. 1597-1605.

Astronomy and Astrophysics

Astronomy

12

Stars: Variables: Cepheids, Globular Clusters: Individual (Ngc 1866), Galaxies: Magellanic Clouds, Stars: Evolution, Stars: Mass Loss

Scientific paper

Available observational data for the 20 known Cepheids in the LMC cluster NGC 1866 have been compared with Hubble Space Telescope observations, discovering in the cluster central region five additional variables, one of which appears to be a Cepheid candidate. We also reach the conclusion that only the photometric data for the seven variables in the cluster periphery appear accurate enough to allow a meaningful comparison with the results of pulsational theories. Out of these seven well-observed Cepheids, we find that the six probable cluster members are located in the color-magnitude diagram at the hot tip of the blue nose experienced by He-burning giants. Since evolutionary theory predicts for these giants an original mass on the order of 4 Msolar, we extend down to ~3 Msolar the theoretical pulsational scenario already presented for M>=5.0 Msolar. On this basis we discuss the four member Cepheids with VI magnitudes accurate enough to produce robust constraints on the pulsating structures. Among these variables, one finds evidence for a spread of masses by about 7%, with the structures following a tight mass-luminosity relation. Moreover, we show that periods and colors of the Cepheids give a robust indication of pulsator masses smaller than predicted by stellar evolution theory without mass loss, independently of the occurrence of core overshooting.

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