Place In Sun Research Articles

The Vision of Billy Wireman

history of innovative higher education has produced its share of charismatic leaders, men and women with strong educational ideals who have managed to convey to their faculty and students a sense of their own importance and of their university's special place in sun. If leadership has been particularly daring and imaginative, leader and college may even become synonymous in people's minds. Such is case with Billy Wireman and Eckerd College, or Florida Presbyterian as it was first called. a real sense, Eckerd College was Billy Wireman, and vice versa. It came down to that, was way one faculty member put it. At beginning of 1960s in St. Petersburg, a city best known for its attractiveness to elderly retirees from Midwest, Presbyterians of Florida had decided to launch a college. It was an unlikely place but a propitious time for start of an institution devoted to youth: Higher education in United States was entering an era of rapid expansion, and Florida, nation's fastest-growing state, was destined to lead way. Propelled by a spirit of infinite possibility in what some now recall wistfully as Age of Camelot, Florida Presbyterian College (FPC) was proclaimed a budding new model of liberal arts excellence. It was dedicated to innovation and relevance long before those terms became hackneyed and meaningless. Less freewheeling than New College, its near neighbor and contemporary in Sarasota (see Change, May 1975), FPC nonetheless nourished a singular vision. It aspired to be church related in a time of growing secularism, small and intimate in a time of pervasive bigness, an amalgam of traditional and latter-day liberal arts ideals in a time of specialization run amok. Billy Wireman epitomized new institution's accent on youth. In early years he was physical education and athletics department, or most of it, and he looked part: Strong, crew cut, ruggedly handsome, he was 28 years old and filled with enthusiasm and energy. He had just completed his doctorate at George Peabody College for Teachers, a d two years before he had been an assistant basketball coach under legendary Adolph Rupp at University of Kentucky when Rupp's charges won NCAA championship. William Kadel, FPC's first president, often spoke of his hope that new College would become the Princeton of South. Kadel and John Bevan, vice president for academic affairs, hand-picked a charter faculty of 22 persons, one for every seven JOHN EGERTON is teaching this year at Virginia Polytechnic Institute. He is a frequent contributor to Change.

Place in Sun for Marston, Downtown for Sherman

Place in Sun for Marston, Downtown for Sherman

Place in Sun for Marston, Downtown for Sherman

Place in Sun for Marston, Downtown for Sherman

Place in Sun for Marston, Downtown for Sherman

Place in Sun for Marston, Downtown for Sherman

Die unterschiedliche Synthese der lipophilen Plastidenchinone in Sonnen- und Schattenblättern von Fagus silvatica L. / The Unequal Synthesis of the Lipophilic Plastidquinones in Sun- and Shade Leaves of Fagus silvatica L.

The synthesis of plastidquinones was studied from leaf development until autumnal leaf degeneration in sun and shade leaves of Fagus silvatica and compared with chlorophyll and carotinoid synthesis. 1. The lipoquinone content of Fagus chloroplasts increases steadily with increasing age of leaf tissue. This lipoquinone accumulation takes place in sun and shade leaves, it is however much more expressed in sun leaves. On a chlorophyll or a leaf square (100 cm2) basis the latter possess a several times (3 to 9 x) higher lipoquinone content than shade leaves. 2. The augmentation of the plastidquinone level in both leaf types is mainly due to the synthesis of the reduced benzoquinone forms, plastohydroquinone 45 and the chromanol a-tocopherol. The larger part of the reduced lipoquinones represent excess amounts which are deposited extrathylakoidal in the osmiophilic plastoglobuli of the plastid stroma. 3. The oxidized benzoquinones, plastoquinone 45 and α-tocoquinone, as well as the naphthoquinone vitamin K1 (phylloquinone) are present in much lower concentration. Their synthesis parallels that of chlorophylls and carotinoids. They are formed either not in excess (vitamin K1) or in very low excess amounts (α-tocoquinone, plastoquinone) . These oxidized quinone forms are in turn preferably located together with chlorophylls and carotinoids in the photochemically active thylakoids. 4. The production of excess plastidquinones (mainly reduced benzoquinones) starts very early during leaf development. The main synthesis phase begins after the end of chlorophyll and thylakoid synthesis and continues in senescent Fagus leaves during the breakdown of chlorophyll and thylakoids until the early yellow stage of sun and shade leaves. In senescent leaves the level of the oxidized benzoquinones, plastoquinone and α-tocoquinone, increases slowly by oxidation of plastohydroquinone and α-tocopherol, respectively. 5. The differences between sun and shade leaves in the total and relative amounts of the various lipid classes such as chlorophylls, carotinoids, benzoquinones and the naphthoquinone K1 (100 cm2 leaf square, dry weight or chlorophyll a as reference system) are not yet significant in May, several days after leaf unfolding, but get established thereafter. 6. By August the benzoquinone content of sun leaves reaches even that of chlorophyll a, whereas in shade leaves the lipophilic benzoquinones make up only 20 to 30% of the chlorophyll a content. Shade leaves exhibit a benzoquinone level which is little lower than that of carotinoids. Sun leaves, in contrast, contain a benzoquinone content which is by ca. 4 times higher than the carotinoid content. The ratio benzoquinones to vitamin K1 amounts 60 - 70 in shade leaves and 100 - 120; n sun leaves. In addition the two lipophilic redox systems plastoquinone/plastohydroquinone 45 and α-tocoquinone/α-tocopherol are present in sun leaves to a higher extent in the reduced state (84% and 96%) than in shade leaves (60% and 90% respectively). 7. From the results it is assumed, that the steady increase of the benzoquinone level with increasing age of plant tissue may be correlated with thylakoid turn-over. The possibility, that the enormous benzoquinone accumulation in sun leaves is mainly caused by higher light intensities in connection with a reduced protein synthesis is discussed.

Technology in the Modern World

The broad field of automation covers, inter alia, my first reaction on being awarded difficult but absorbing task of addressing you on Technology in Modem World. I turned automatically and confidently to Encyclopaedia Britannica of 1962 and read avidly every reference indexed under Here it is, verbatim: Moreover, settled agricultural life needed more tools, at first of stone. Thus a professional technology developed. The rest is silence. I moved my calendar back to 1961, not without gain. For Encyclopaedia Britannica 1961 said this: Moreover, settled agricultural life needed more tools, at first of stone. Thus a professional technology developed. Both, however, do condescend to particular in describing technological as the higher levels at which advanced knowledge of theory is important -this in contrast to technical education directed primarily at acquirement of skills in techniques. Compare these fragments, however, with their counterpart in great Eleventh of 1910-11, Philip Magnus on Technical Education together with biographic note on Johann Beckmann (1739-1811) who-in 1772-invented title of Scientific Technology. We are, I hope, going to change all this imbalance. As an unrepentant technologist, I hereby dedicate all effort for which anyone is prepared adequately to pay me, to giving technology its place in sun. In sunshine, that is, of an Encyclopaedia Britannica which should surpass even high standards of an epoch when E signified Edinburgh as well as Encyclopaedia. I do not attempt difficult task of defining my terms; I can approach them only by indirection. Science and technology are Gemini of (not always heavenly) conceptual constellations of human mind. They are far from identical twins, and endless confusion may be generated by failure to recognize their sharply differentiated identities. They are, however, like Siamese twins; they share a common blood stream, but are divergent in their outlook on their common world. This divergence of outlook denies them status of heavenly twins-science may pretend to adjective, but technology is of earth, earthy.

Atomic Fission Takes Place in Sun's Corona, Is Theory

Atomic Fission Takes Place in Sun's Corona, Is Theory

The Night Sky in June

THE nights around the summer solstice on June 21 are shorter than 7J hours in the latitude of London, reckoned from sunset to sunrise; excluding twilight (nautical) darkness lasts only about three hours. The moon is new on June 6 and full on June 19. Venus, which is still a brilliant evening star at the beginning of the month, draws rapidly towards the sun's place and is at inferior conjunction on June 26. Mercury is also an evening star in conjunction with Venus on June 12 and with Mars on June 17; on June 24 Mercury is at greatest elongation (25° east). Mars is getting less easy to see; it is close to Venus on June 7. Jupiter and Saturn are both morning stars, the former rising soon after lh. 30m. U.T. on June 16, followed ihr. later by Saturn. At dusk in mid-June, the red star Antares is about south. Arcturus has already southed, while Vega is some 3 hours before the meridian. The constellations, Bootes, Hercules and Ophiuchus contain some interesting double stars of which e Bootis (2-8″), Bootis (·1″)> a Herculis (4-8″) and 70 Ophiuchi (6-6″) are good examples. Between A and B Herculis may be glimpsed with the naked eye under favourable conditions the great star cluster, ?13, the distance of which is of the order 35,000 light years. The outer part of the cluster can be resolved into stars with a 2-B- or 3-inch refractor. The Scorpiid meteors are at their greatest frequency about June 4, their radiant point being north, following Antares.

The Sun's Place in the Universe

The Sun's Place in the Universe

The Sun's Place in the Universe

The Sun's Place in the Universe

The Sun's Place within the Star-sphere

The Sun's Place within the Star-sphere

The Sun's Place in Nature . By Sin Norman Lockyer. London and New York, The Macmillan Company. 1897. Pp. 360. Price, 12 shillings.

<i>The Sun's Place in Nature</i> . By Sin Norman Lockyer. London and New York, The Macmillan Company. 1897. Pp. 360. Price, 12 shillings.

The Sun's Place in Nature1: XI

The Sun's Place in Nature1: XI

The Sun's Place in Nature1: X

The Sun's Place in Nature1: X

The Sun's Place in Nature: IX

IN most of the earlier attempts which were made to explain the origin of new stars, the leading idea was that of a single body being suddenly disturbed in some way, with the possible result that the heat of its interior became manifested at the surface. Thus Zöllner, in 1865, suggested that the phenomena might be produced by the bursting of the crust which had just formed on the surface of a star approaching extinction. Again, in connection with the new star in Corona, I pointed out in 1866 that all that seemed necessary to get such an outburst in our own sun was to increase the power of his convection currents, which we know to be ever at work. Dr. Huggins at that time believed that the appearances were due to gaseous eruptions in a single body, and that “possibly chemical actions between the erupted gases and the outer atmosphere of the star may have contributed to its sudden and transient splendour.”

The Sun's Place in Nature:1 VII

AT the end of the last lecture, some evidence was brought forward which leads to the conclusion that in those stars in the spectrum of which bright lines are seen, we are dealing with bodies closelv, associated with nebulæ. It was at once suggested that possibly by those new methods of inquiry to which I have already referred, we might be enabled to demonstrate the existence of the nebulæ, although we can never hope to see them by the unaided human eye. The idea occurred to me that long exposed photographs might give us stars surrounded by nebulæ.

The Sun's Place in Nature:1 VI

The Sun's Place in Nature:1 VI

The Sun's Place in Nature1

The Sun's Place in Nature1

The Sun's Place in Nature1

III. THE next question that we have now to consider has to do with the connection between nebulæ and stars, and I shall show that the more the facts are studied the closer does this connection prove to be. You remember that that was the idea which lay at the bottom of the hypotheses both of Kant and of Laplace. In the last lecture I referred to some of the earliest observations which had been made of the nebulæ by means of the spectroscope, and it so happened that Dr. Huggins, to whom we owe this work, came to the conclusion that the result of his inquiries was rather to show that this connection, which had been asserted both by Kant and Laplace, and which had been accepted by everybody up to then, really did not exist. In a paper which detailed these spectroscopic observations, published in 1865, Dr. Huggins stated his conclusion that the nebulæ, instead of having anything whatever to do with any evolutionary line along which both nebulæ and stars might be traced, possessed a structure and a purpose in relation to the universe altogether distinct and of another order. So that you see the first apparent teaching which we got from the spectroscope practically put us in a very considerable difficulty; if it had to be accepted, of course the views of Kant and Laplace would have to be rejected.

The Sun's Place in Nature

IV. THE difference in the appearance of spectral lines and flutings having been explained, I now go on to state that the luminosity referred to, as seen in the meteorite experiment was not one of the lines in the spectrum of magnesium, but one of the flutings. I will next throw this on the screen (Fig. 17), and you will at once see the point. Here is the spectrum of magnesium obtained at the lowest temperature at which we can get any light from it at all. We have a fluting, which resembles closely the carbon fluting, but in a different part of the spectrum. We see that its brightest part is coincident with a certain part of the solar spectrum; and it so happens that the position of the line which Dr. Huggins had observed in the nebulæ lies very near the same position of the solar spectrum.