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• W807001644 abstract "Virginia Trimble What I want to try to do in the next few pages is to review the history of the Universe from the earliest times for which we have any evidence down to the present day, with special em- phasis on how conditions favorable for life seem to have arisen, and then to explore the extent to which this history is dependent upon the Uni- verse having roughly the properties it does, and finally to inquire into the implications of varying those prop- erties. A Cook’s tour of the universe and its early history Let’s start by taking a look (Table 1) at the scales of the things we will be discussing. Notice that the human scales in each case are close to the geometric means of the astronomical and atomic scales. Thus, we should not be surprised to find that our presence here is dependent both on Virginia Trimble is grateful to the Aspen Center for Physics, where much of this was written, for hospitality, and to the Alfred P. Sloan Foundation for a Research Fellowship (1972-74). The author&#39;s thoughts on the Universe and its contents have inevitably been influenced by more people than can conve- niently be mentioned, but those from whom she first heard some of the ideas discussed here, and whom she would therefore like to thank especially, include Dave Arnett, Wil- liam A. Fowler, Jim Gunn, Philip Morrison, Paula Moddel, Bohdan Paczyriski, Martin Rees, Bill Saslaw, Starling Trimble, and (last only in this deliberately alphabetical list) Joe Weber. Address: Department of Physics, University of California, Irvine CA 92717 (January to June); Astronomy Program, University of Maryland, College Park MD 20742 (July to December). 76 American Scientist, Volume 65 Cosmology: Man’s Place in the Universe In which we review the history of the Universe and explore the relationships between its properties and the presence of life the large-scale phenomena of as- tronomy and on the details of atomic physics. The largest phenomenon of all is, of course, the Universe itself. It is im- portant to be sure we agree about what we mean by “the Universe” and the various other terms we will be using. The earth and eight other planets, about 34 moons, and a vari- ety of smaller objects are in gravita- tionally bound orbits around a star called the sun. We refer to this grouping as the Solar System. It has a total mass of about 2 X 1033 grams (virtually all in the sun, though most of the angular momentum is in the planets), a diameter of about 2 X 1015 cm, and an age of about 5 X 109 yr. The sun is a perfectly typical star, having a mass of 2 X 1033 g (the solar mass, abbreviated Me, is often used as a unit for other stars), an electro- magnetic radiation energy output of 4 X 1033 ergs/sec (one solar luminos- ity, Le), a spectrum approximately that of a 5700 K black body, a radius of 7 X 10q’ cm (1 R9), and a compo- sition by weight (at least in its outer, visible layers) about 73% hydrogen, 25% helium, and 2% everything else (about half of it carbon and oxy- gen). The sun, in turn, is one of about 2 X 10“ stars that are gravitationally bound in a rotating, roughly spherical system (although the most conspic- uous members are concentrated in a plane considerably flatter than the proverbial pancake) called the Milky Way Galaxy (or just the Galaxy). It has a mass of at least 3 X 1044 g (but see Ostriker et al. 1974 for evidence that it may be ten times more massive than this) and a diameter of about 1023 cm. It is at least 10q’ yr old. The Milky Way, in turn, is bound in a small cluster of about 30 galaxies (all but one much less massive than ours) called the Local Group. It is not certain whether higher-order struc- tures are gravitationally bound, but there does seem to be some clustering of the clusters (Hauser and Peebles 1973). The clusters range from small ones like the Local Group up to much richer ones containing thousands of galaxies and having masses of 10‘5 M9. Completely isolated galaxies are probably rare (Tifft and Gregory 1976). The properties of the medium between the galaxies (except within the rich clusters, where a hot intra- cluster gas is often a strong source of X rays; Kellogg et al. 1973) are very poorly known. The average density could be anywhere from 0 to 1O‘5 particles cm‘3, the intergalactic me- dium comprising anywhere from 0 to 90% of the total average density over large regions of space. If the density is high, the matter must also be rather hot (~1O6 K) or exceedingly clumpy to prevent detection. A preponder- ance of the evidence (as summarized, e.g., by Gott et al. 1974) now seems to favor an intergalactic density at the low end of the possible range. The clusters of galaxies (or perhaps the superclusters) appear to be dis- tributed at random through space, with separations such that they con- tribute an average density of at most 10‘31 g cm‘3 (Ostriker et al. 1974). There is no detectable falloff of the density of clusters of galaxies out to the largest distances at which they can be seen with present telescopes. This is about 1023 cm or 3000 Mpc (Megaparsecs; one parsec = distance at which an object has a parallax of one second of arc = 3 X 1013 cm), corresponding to a light travel time of" @default.
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• W807001644 title "COSMOLOGY - MANS PLACE IN UNIVERSE" @default.
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