Photograph used for a story in the Daily Oklahoman newspaper. Caption: "Vietra Watson and Derrick Wilson, front, plant rotunda holly while Ed Reeden, landscape designer with Oklahoma Public Schools, and Alice Johnson, of the Cleveland Neighborhood Association watch."

Photograph used for a story in the Daily Oklahoman newspaper. Caption: "Mrs. Wilbur (Kay) Jones, City"

Photograph used for a story in the Daily Oklahoman newspaper. Caption: "Wilbur checks one of the two 18-unit purple martin houses he built and installed in his back yard."

Photograph used for a story in the Oklahoma Times newspaper. Caption: "Moore adult services librarian Maureen Goldsberry puts the finishing touches on the library's calligraphy exhibit."

Photograph used for a story in the Daily Oklahoman newspaper. Caption: "Debbie Guin of Mustang is the first-place winner in the "Great MS Take-Off."

Photograph used for a story in the Oklahoma Times newspaper. Caption: "Curtis Fortenberry is moving about 25 homes along Grand Blvd."

Photograph used for a story in the Oklahoma Times newspaper. Caption: "HEAD HIM OFF AT THE PASS --- Odell Carson of Star-Spencer's tries to cut off Muhammad Akbar of U.S. Grant before he can pass to a teammate.."

Photograph used for a story in the Daily Oklahoman newspaper. Caption: "SW's Kelli Litsch (30) meets Shelly Brown"

Many of the upper main-sequence stars pulsate in spheroidal nonradial modes. We know this to be true in numerous cases, as we have tabulated for the ..beta.. Cephei and delta Scuti variables in previous lectures. However, we cannot identify the actual mode for any star except for the low-order pressure p and f modes of our sun. It remains a great challenge to clearly state what really is occurring, in the process we learn more about how stars evolve and pulsate.

The properties of a coaxial magnetocumulative generator (MCG) in which the current increases exponetially with time are derived and discussed. Such an exponential MCG possess highly desirable performance characteristics that are readily derived and expressed in terms of simple formulas. It is concluded that an exponential MCG may approach a capability of delivering 100 megajoules to a 1 nanohenry load in 1 microsecond.

Video footage from the KXAS-TV/NBC station in Fort Worth, Texas, to accompany a news story.

Video footage from the KXAS-TV/NBC station in Fort Worth, Texas, to accompany a news story.

Video footage from the KXAS-TV/NBC station in Fort Worth, Texas, to accompany a news story.

Video footage from the KXAS-TV/NBC station in Fort Worth, Texas, to accompany a news story.

B-roll video footage from the KXAS-TV/NBC station in Fort Worth, Texas, to accompany a news story.

In this study of stellar structure, evolution, stability, and pulsation or explosion, there are three very vital pieces of physical information needed. We assume the composition is known from observations of assumption. To construct a model of a star we then need to know the nuclear generation rates which give the luminosity the star emits, the pressure and energy equation of state which determines the flow of radiation through the star. It is the equation of state and opacity that we will be discussing in the next two lectures.

Spectral variations of the class of variable stars that seems to have no radial pulsations at all are discussed. Models of the rotation of these stars are considered. (GHT)

The stars that we consider here have luminosities above 10,000 solar luminosities and masses above 15 solar masses. We contact the 53 Per stars such as ..nu.. Ori, 10 Lac, and iota CMa at our lower luminosity limit, and at the most luminous limit, we have the famous stars eta Car, Cyg OB12, and P Cyg. Evolution tracks including a reasonable mass loss rate are given for 15, 30, 60, and 120 solar masses. It appears that our pulsators have masses less than 60 solar masses, but how do the most luminous stars observed survive mass loss. Do they have masses above 100 solar masses as indicated, or are these stars somehow superluminous due to their erratic mass loss behavior. Popper (1980) studying the masses in binary systems has never found one with a value greater than 27 solar masses.

Environmental monitoring efforts spanned air, water, vegetation and foodstuffs, and radiation doses. Monitoring data collection, analysis, and evaluation are presented for air, soils, sewage, water, vegetation and foodstuffs, milk, and general environmental radioactivity. Non-radioactive monitoring addresses beryllium, chemical effluents in sewage, noise pollution, and storm runoff and liquid discharge site pollutants. Quality assurance efforts are addressed. Five appendices present tabulated data; environmental activity concentration; dose calculation method; discharge limits to sanitary sewer systems of Livermore; and sampling and analytical procedures for environmental monitoring. (PSB)

A very sophisticated method for calculating the stability and pulsations of stars which make contact with actual observations of the stellar behavior, hydrodynamic calculations are very simple in principle. Conservation of mass can be accounted for by having mass shells that are fixed with their mass for all time. Motions of these shells can be calculated by taking the difference between the external force of gravity and that from the local pressure gradient. The conservation of energy can be coupled to this momentum conservation equation to give the current temperatures, densities, pressures, and opacities at the shell centers, as well as the positions, velocities, and accelerations of the mass shell interfaces. Energy flow across these interfaces can be calculated from the current conditions, and this energy is partitioned between internal energy and the work done on or by the mass shell. We discuss here only the purely radial case for hydrodynamics because it is very useful for stellar pulsation studies.

A technique was developed to determine the rate and equilibrium constants for the base-catalyzed exchange of tritium from ehavy water to deuterochloroform. An activation energy and entropy were also calculated. These quantities are comparable with those reported in the literature for a similar reaction involving the exchange of deuterium from deuterochloroform to water. It was found that the exchange reaction occurred predominately between the dissolved reactants in the D/sub 2/O and CDCl/sub 3/ phases. The rate constant is a strong direct function of temperature while the equilibrium constant is a weak inverse function.

In discussing upper-main-sequence stars and their intrinsic pulsations, we need to realize that theory has not yet been able to understand these pulsations. In many discussions the character of the pulsations has been described, and in many cases these theoretical solutions of the stellar pulsation theory may be the actual ones occurring. But the specific driving mechanism, so well known for the yellow and red giants and supergiants, and very recently known for the white dwarf stars, remains the subject for intense discussion. My ideas will pervade all my discussion, but many of them concerning the details such as the cause of the pulsations have not yet been proved correct.

Moving down the main sequence from the ..beta.. Cephei variables, we come to later B-type stars. The suspicion of variability for these stars goes back to Vogel in 1891 who studied the radial velocities of Vega. Since that time there have been numerous studies of Vega (Wisniewski and Johnson 1979, Fernie 1981) and other B and early A stars which hint at variability in both radial velocity and light. Since Struve (1955) discussed these stars 28 years ago, they have been called the Maia stars after the Pleiades star that he thought was the prototype. The uncertainty in their actual variability has led Breger (1980) to call them the mythical Maia variables.

We turn to the effects on opacities of atomic lines and molecular bands. It was the realization that these atomic lines were important for the opacity and the radiation flow in stars that allowed the field of stellar evolution to greatly flower in the 1960's and 1970's. Our understanding of stellar structure and evolution is now very deep.