EDP Sciences
Free Access
Volume 395, Number 1, November III 2002
Page(s) 69 - 75
Section Stellar clusters and associations
DOI https://doi.org/10.1051/0004-6361:20021220
Published online 29 October 2002

A&A 395, 69-75 (2002)
DOI: 10.1051/0004-6361:20021220

Helium variation due to self-pollution among Globular Cluster stars

Consequences on the horizontal branch morphology
F. D'Antona1, V. Caloi2, J. Montalbán1, P. Ventura1 and R. Gratton3

1  INAF, Osservatorio Astronomico di Roma, via di Frascati 33, 00040 Monteporzio, Italy
2  Istituto di Astrofisica Spaziale e Fisica Cosmica CNR, via Fosso del Cavaliere, 00133 Roma, Italy
    e-mail: caloi@rm.iasf.cnr.it
3  INAF, Osservatorio Astronomico di Padova, vicolo dell' Osservatorio, 5, 35122 Padova, Italy
    e-mail: gratton@mostro.pd.astro.it

(Received 19 June 2002 / Accepted 23 August 2002)

It is becoming clear that "self-pollution" by the ejecta of massive asymptotic giant branch stars has an important role in the early chemical evolution of globular cluster stars, producing CNO abundance spreads which are observed also at the surface of unevolved stars. Observing that the ejecta which are CNO processed must also be helium enriched, we have modelled stellar evolution of globular cluster stars by taking into account this possible helium enhancement with respect to the primordial value. We show that the differences between the main evolutionary phases (main sequence, turn-off and red giants) are small enough that it would be very difficult to detect them observationally. However, the difference in the evolving mass may play a role in the morphology of the horizontal branch, and in particular in the formation of blue tails, in those globular clusters which show strong CNO abundance variations, such as M13 and NGC 6752.

Key words: stars: abundances -- stars: horizontal branch -- globular clusters: general

Offprint request: F. D'Antona, dantona@coma.mporzio.astro.it

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© ESO 2002

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