Illinois Junior Academy of Science - Yearbook (Urbana, IL)

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The above students represented the IJAS at the AAAS meeting, where they presented their papers. Left to right: Larry Lunardl, Lynn Grandt, Sister Mary Alvernla.. -xv S. s mai gi-an N 'ms ft H5 : f - Pamela. Carsan Western High School, Macomb

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ILLINOIS SOCIETY FOR MEDICAL RESEARCH ESSAY CONTEST I ITSBCIIBFS are indicated in parenthesesl PLACE: 1. Kristine Lapp, Nazareth Academy, La- Grange Park CSishter Donna Mariel 2. Theodore S. Wright, Jr., Oak Park and River Forest H. S., Oak Park fJoseph P. McMenaminJ 3. Stephen R. Miller, New Trier, H. S., Win- netka fLoris A. Hoytl 4. Kathie Flynn, Mercy H. S., Chicago CSister Mary Josita, R.S.M.J 5. Janett Works, Egyptian H. S., Thebes CJames Flattj HONORABLE MENTION Un aIpI1abeiicaI orderl Sheila R. Castillo, St. Mary H. S., Chicago fSister Mary de Lourdesj Barbara Downing, Taft H. S., Chicago, CMr. Gierschj Robert G. Eckley, Peoria H. S., Peoria 1Miss Gama Kinhoferl Linda Gray, Cullom H. S., Cullom fMr. Work- manl Janet Hickey, Immaculate Conception H. S., Elmhurst CSister M. Rosalinal Janet Jarke, Immaculata H. S., Chicago CSis- ter Mary St. Eulalial Stella Kaszuba, St. Stanislaus Kostka H. S., Chicago QSister Mary Lucinaj 6. Brenda Likes, Bluffs H. S., Bluffs fMrs. Don Bunchj Suzanne Ostlund, Nazareth Academy, La- Grange Park fSister Evangelistj 8. Nancy Hoff, Immaculate Heart of Mary H. S., Westchester QSister Rose Anthonyl 9. Peggy Cullerton, St. Francis H. S., Wheaton CSister J udel 10. Jean Tille, Stephen Decatur H. S., Decatur fMr. Thistlethwaitej Mary Kay Kilburg, Immaculate Conception H. S., Elmhurst CSister M. Rosalinal Jan Mayer, Deerfield H. S., Deerfield CRobert Torsbergj Barbara Parrish, Carbondale Community H. S., Carbondale fMr. Lawrencel Stuart B. Piper, Lyons Township H. S., Wes- tern Springs fKenneth Nelsonj Judy Rosenberg, New Trier H. S., Winnetka CMr. Loria A. Hoytj Catherine Sanborn, St. Benedict H. S., Chi- cago iSister John Teresej Alice Wernsing, Beecher City H. S., Beecher City fWilliam Squires! Susan Wolfe, New Trier H. S., Winnetka fMr. Loris A. Hoytl FRANK REED AWARD Steven C. Carhart Prof. C. K. Hunt Left to right: Kristine Lapp, lst place awardg Jean Tille, 10th place award: Suzanne Ostlund, 7th place awardg Kathie Flynn, 4th place award.

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Sawclust Effect On Tilth f LYN GRANDT , LaGrove High School I l Farina PURPOSE The purpose of my project was to observe the effects of sawdust and ammonium sulphate on the tilth of the soil under several normal conditions. PROCEDURE In working witnh my first set, I 'took thirty-five soil sam- ples from seven different locations. In each I put one table- spoon of sawdust and one-half teaspoon of ammonium sul- phate. In seven I planted corn: in seven, alsike clover. To one set, I added earthworms. In one set, I added neither plants nor earthworfns. All four sets were watered. For the control, a fifth set, unplanted and containing no earth- worrns, was left dry. In doing set two, I repeated the procedure followed in doing set one, but the following additions were made: seven cartons containing soil, sawdust, and ammonium sulphate were planted with corn and alsike clover. Earthworms were added to seven more cartons containing soil, sawdust, ammo- nium sulphateg corn and alsike clover were planted in these. To seven more cartons of untreated soil, I added gypsum. All additional groups received water. I ' RESULTS I received very good results on my first set. The earth- worms made the soil more porous for better tilth. There was much variation in the growth of the corn and alsike clover. Some of the soil became very tightly packed. The Study ot Mass Interchange in Binary Systems ROBERT McNAMARA Brother Rice High School Chicago Brother M. R. Kelleher In this study it was my aim to research mass interchange in binary star systems. My study, though, was not concerned with the actual observation of these systems, but of the forces that control the mass transfer process and how mass transfer affects the system. With this in mind, I limited myself to the fact that mass transfer exists and then I tried to determine under which conditions mass transfer can oc- cur, the reason for its occurrence, and how it effects the behavior of different star systems. The first consideration in the study of mass transfer is to define a surface to which the infinitismal particle of the star is to be restricted. This can be defined by the equation: X'-l-y'+ 2.1-1 -M- .2..M. rt + rl 2 C where the two masses are A defined and 1 -,Ll , respectively, and rotating axis having been chosen with the center of mass as the origin. The x axis is the line joining the two masses. Once C is stated the surface it defines is called the equipotential or zero-velocity surface. This surface divides space into two spaces, one accessible and the other inacces- sible to the infinitismal particle. The exact shape of this surface depends on the value of C. For large C the zero velocity surfaces differ only slightly from separate closed spheres. For decreasing C they become more elongated until they touch at some common point on the x axis, L.. For smaller C, a single zero velocity surface surrounds the two bodies, and for even smaller C, the dumb-bell increases in size and finally opens up at point L2 and finally Ls. Particles placed at these points are free of gravity and will remain at rest unless perturbed by external forces. L2 and L3 control the mass flow out of the system and Ll is the route for transfer. The equipotential surface or zero-velocity surfaces are the keys to the mass transfer process. In close binary sys- tems the lobes meet at a common point, L., along the x axis. In the systems with data leading to the fact of mass inter- change, it is speculated that the primary in the system be- gins to evolve and it starts to fill its equipotential lobe. This expansion is very rapid, because if the primary is to reach its Roche limit, it must go through the Hertzsprung gap. This rapid evolution quickly expands the radius of the pri- mary and the star fills its lobe. But, the tendency for ex- pansion remains, and the gases on the outer layers escape through the only possible outlet, L, As the mass flows into the lobe of the secondary, it takes up orbit around the sec- ondary and forms a shell or ring around the star. Some of the mass may escape the system at points La and Ls, but this depends on the value of C. Now we come to our first major difficulty. Spectro- scopic observations of the 70 or 80 close binary systems have found that in systems with mass transfer it is always the secondary and not the primary which has filled its lobe to the Roche limit and is transferring the mass to the other lobe of the system. This situation can be explained by the hypothesis of Donald C. Morton, which states that the pri- mary does evolve first, fills its surface, and transfers enough of its mass to its other companion so as to exchange the roles of primary and secondary. fThis does not include very close systems, i.e., W. Ursa Majoris.J Plotting of the Roche limits of typical systems on the H - R diagram shows tlhe primary can only reach its limit in the Hertzsprung gap, where even normal evolution is relatively fast. However, for this to be valid it must be accomplished in a process that its chances of being observed during the transmutation are small. This transition has been found to be fast enough so that few sys- tems could be caught making it. First, we start with a nearly homogenous primary in one of the various phases of evolution that is in a nuclear time scale. The nuclear time being stated for the star by the equation: rn L log T815 I 10.1 + log Fig -' log T19 If, during this interval, the star goes into a phase lasting a Kelvin Time, the Kelvin Time for the primary being de- fined by: m .Is log Tau I 7.7 + log me - log Lg K then we would expect to see less than 1111 of the group mak- ing the transmutation since the Kelvin Time is shorter by a factor of 200. Also, since the rate of transfer during the instability is governed mainly by the time it takes the outer layers to reach thermal equilibrium, the Kelvin Time may be somewhat shorter than for that of the whole star. Sta- bility returns in the expansion when t-he star loses so much mass as to approach homogenity with a Hydrogen poor com- position. But, this happens after the exchange of the role of primary and secondary. This accounts for about all observations except those of secondaries only partially filling their lobes, but this is more than likely due to a different composition, in which the sec- ondary lacks a Hydrogen rich envelope. It may be expected eventually that the new primary will start to evolve and return some of the mass that came from it originally. tStruve, 19443 CHoylel There has been much speculation as to how mass effects the evolution of a close binary system. An example would be Mr. Robert P. Kraft's suggested evolution of a W Ursa Majoris star to a U Geminorum star. These stars would not apply to Mr. Morton's theory due to their extreme closeness and their age. They seem to be older than the ordinary mass transferring binary or are in a later evolutionary phase. Mr. Kraft's whole theme rests on the findings of Huang t1956l that in a binary system, if a star loses mass to its 1 4