By Jun Jugaku (auth.), M. Spite (eds.)

This ebook includes the lawsuits of the 1st 'Rencontres de l'Observatoire' which used to be held on the Meudon campus of the Paris Observatory on September 21-25, 1998. the topic addressed was once 'Galaxy evolution: Connecting the far-off Universe with the neighborhood fossil record'. This colloquium used to be a undertaking devised via a bunch of astronomers who, in France but in addition in Europe, within the usa, in South the US, or even in Japan, have labored for a very long time with Roger and Giusa Cayrel. Roger and Giusa had a major effect on us all. They taught us of their discrete approach, the care of the observations and the rigor within the interpretation. along with the shows of Jun Jugaku and Rene Racine and the presentation of Pierre Couturier of the tale of the Canada-France-Hawaii Telescope (presentation which regrettably doesn't seem during this booklet) numerous papers consult with the position of Roger and Giusa in astronomy. Their contribution to the examine of the galactic evolution has been basic. Our Milky method is the galaxy that are studied in so much information. From the research of our Galaxy's outdated inhabitants, one could comprehend what our Milky method was once like very quickly after its beginning, on the related level the place we now discover the very far away and hence very 'young' galaxies. The organizers desired to collect with Roger and Giusa Cayrel specialists of the outdated Galactic inhabitants, of the far away galaxies and of the galactic evolution.

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Extra resources for Galaxy Evolution: Connecting the Distant Universe with the Local Fossil Record: Proceedings of a Colloquium held at the Observatoire de Paris-Meudon from 21–25 September, 1998

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This fact implies that the surface layers of the brighter stars must have been brought to temperature high enough to complete the full CNO cycle, thereby burning 3He into 4He. This, in tum, implies an extra dredge-up episode plausibly taking place after the 'Red Giant Bump'. The present value of 12C/l3C in ISM is ~ 50, appreciably larger than the protosolar value of 90. One question comes to mind: what is the contribution of this new episode to the ISM value of l3C? A simple estimate can be obtained in the following way.

What limits our ability to accurately simulate their behavior? These and related questions are critically reviewed. 1. Introduction Within a Big Bang cosmology there must be an epoch at which the first stars formed. , elements carbon and above), which can now be observed in the most metal-poor stars and plasma. Theory of this nucleosynthesis is deeply entwined with the assumptions used to model the evolution of these stars. One of the first indications of early stellar nucleosynthesis was the 'alpha effect' (Greenstein, 1970; Wallerstein, 1968), in which the abundance of the 'alpha elements' such as (0, Mg, Si, S, Ca and Ti) is high relative to Fe in the most metal-poor stars.

The shock advances easily within the Stromgren sphere, but is strongly decelerated outside the sphere because it has to ionize the matter there. Thus the shock radius is likely to coincide with the Stromgren radius, which depends on both the progenitor mass and the number density of hydrogen in the ambient ISM per cubic centimeter, no. We estimate that the hydrogen mass swept up by the shock is 4 x 104 . 0)-1 Mo for M = 25 M o and 4 x 103 . 0) - 1 M o for M = 15 M o , using low metal progenitor models.

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