By B. Baldwin

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S. and Rosner, R. 1978, Annual Review of Astronomy and Astrophysics, 16, 393. Webster, B. and Murdin, P. 1972, Nature, 235, 37. gov Abstract The ejecta of the first probably very massive stars polluted the Big Bang primordial element mix with the first heavier elements. The resulting ultra metal-poor abundance distribution provided the initial conditions for the second stars of a wide range of initial masses reaching down to intermediate and low masses. The importance of these second stars for understanding the origin of the elements in the early universe are manifold.

465-466. Giacconi, R. 1974, “Binary X-Ray Sources”, Proceedings of IAU Symposium No. 64 (D. , 1974) pp. 147-180. Giacconi, R. and Rossi, B. 1960, J. of Geophys. Res. 65, 773. Giacconi, R. B. 1960, “A brief review of Experimental and Theoretical Progress in X-ray Astronomy,” Technical Note of American Science and Engineering, ASE-TN-49, Jan. 15. et al. 1965, Nature 207, 573. Giacconi, R. et al. 1962, Phys. Rev. Letters, 9, 439. , et al. 1969, Space Science Reviews 9, 3. Giacconi, R. et al. 1971, ApJ 165, L27.

Herwig et al. (1997) were the first to propose that the solution could be non-standard mixing during the AGB evolution. 1), but they also show higher C and in particular O abundances in the PDCZ. Subsequently, Herwig (2000) has explored in detail how the various abundances depend on the overshoot efficiency and other details. In essence, overshooting brings AGB intershell abundances of He, C and O in very good quantitative agreement with the observed abundances of Wolf-Rayet type central stars and PG1159 stars, in the framework of the born-again evolution.

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