The Age of the Oldest Globular Clusters

Astronomy and Astrophysics – Astronomy

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In the paper "The Age of the Oldest Globular Clusters" by M. Salaris, S. Degl'Innocenti, and A. Weiss (ApJ, 479, 665 [1997]), an incorrect statement about the consistency of theoretical values for the core mass at the helium flash was made at the end of the fourth paragraph of § 2.3. This paragraph should be replaced by the following text: Regarding the method that we used, the uncertainties related to the theoretical models of horizontal-branch stars are of concern. It is clear that we do not understand HB morphologies in detail. However, this concerns mainly the distribution of stars along the horizontal direction. For the Delta (V) method, the luminosity, and in our case that of the ZAHB, is the important quantity, and this seems to be much better defined. HB luminosities depend primarily on MHe, which is a very stable quantity in canonical evolutionary models of comparable input physics. Although there has been some discussion about differences of up to 0.02 M&sun; between Mazzitelli (1989) and Sweigart (1994), recent generations of stellar models agree well in predicting MHe, although the adopted physical input is not completely identical. For the standard case of M = 0.8 M&sun;, Z = 0.0001, and Y = 0.23, Mazzitelli, D'Antona, & Caloi (1995) find MHe = 0.512 M&sun;, Salaris, Chieffi, & Straniero (1993) find 0.511 M&sun;, Haft, Raffelt, & Weiss (1994) find 0.503 M&sun;, Weiss (1997, private communication) finds 0.510 M&sun;, and the present result is 0.506 M&sun;. Cassisi et al. (1997) find, depending on different sets of input data concerning EOS, opacities, neutrino emission, and triple alpha -rate values between 0.505 and 0.515 M&sun;. In particular, it has been shown that the latest OPAL opacities and neutrino emission rates result in the higher values quoted. Two entries should be added to the references: (1) Cassisi, S., Castellani, V., Degl'Innocenti, S., & Weiss, A. 1997, A&AS, submitted; (2) Haft, M., Raffelt, G., & Weiss, A. 1994, ApJ, 425, 222.

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