Our group has built a laser system that produces intense light pulses lasting a few tens of femtoseconds. By concentrating the laser energy into such a brief interval, extraordinary intensities can be achieved (equivalent to taking all of the sunlight striking the Earth and concentrating it onto the head of a pin). For more information visit http://webs.byu.edu/jpeatross/ . In one example project, students will use high harmonic light to probe the reflectivity of multi layer mirror surfaces in the extreme ultraviolet wavelength range. Since the high harmonics are linearly polarized, the reflectance at oblique incidence can be studied as a function of polarization orientation.
Students will learn how to safely use high-energy short-pulsed lasers, generate high harmonics, model ultra-short light pulses, use high vacuum systems, and utilize optical detection systems.
Students in our group use intense particle beams (e.g. electrons, x-rays, neutrons) to probe atomic structures in useful and exotic materials such as high-temperature superconductors and superionic conductors and their relationships to the interesting material properties. Our group has a high-intensity single-crystal x-ray diffractometer equipped with a megapixel x-ray camera. We also travel to national and international facilities for synchrotron x-ray and neutron scattering experiments. See http://www.physics.byu.edu/faculty/campbell/ for more information.
Work in computational plasma and gas dynamics involves the kinetic theory of plasma vibrations and applied work on the expansion of a hot gas through a supersonic nozzle. Students who work in this area will learn the basics of particle-in-cell simulations, electrostatic field calculations, and the Direct Simulation Monte Carlo method.
Students will characterize optics designed for the extreme ultraviolet (XUV) part of the spectrum. From these characterizations, we will learn the optical and materials properties needed to design mirrors, filters, and polarizers for applications in space-based telescopes, XUV photolithography, XUV microscopes, and plasma diagnostics. Our analysis tools and techniques include x-ray photoelectron spectroscopy, XUV reflectometry, visible and UV ellipsometry, x-ray diffraction, atomic force microscopy, and electron microscopy. Most of these measurements will be made at BYU, but some may require a trip to the Advanced Light Source at Lawrence Berkeley Laboratories.
For more information see http://volta.byu.edu/xray.html
Our group studies how materials change when they are alloyed with other materials. What happens when a tiny bit of copper is added to aluminum? What happens when titanium is mixed half-and-half with molybdenum? Why does a little bit of scandium harden aluminum? Our studies are computational, numerically solving the Schroedinger equation for a solid, either directly with "first-principles" =approaches or by "fast Hamiltonian" methods such as lattice-based models. Our research often leads us into algorithm development, learning about group theory or combinatorial methods, or developing methods for visualizing or analyzing complex data sets. To see student projects that have been published, go to http://msg.byu.edu/pubs.php.
Our group is working on microscale and nanometer scale fabrication and characterization. Recent advances now allow us to fabricate structures including biological structures with sizes down to a few nanometers across. In our research, we are exploring carbon nanotube composites, nanoscale chemical patterning of surfaces, and nanocrystaline phase change materials. These nanostructures have unique mechanical and electrical properties and will have significant impact in many fields including: solar power conversion, micromachines and mimcrosensors, and biological tissue growth. We perform a host of measurements on these structures to aid in understanding and controlling their structure and physical properties.
There are several opportunities for collaborative research with faculty and current graduate students in the area of acoustics. Many projects involve making a variety of acoustical measurements in different types of sound fields. Examples include pressure or energy-based measurements in our anechoic or reverberation chambers, in ducts, or outdoors. Some research may include working with theoretical or numerical models for comparison with experimental data. Other research could involve measurement automation using LabVIEW or another package. Applications of current research involve architectural and audio design, jet and rocket noise simulation, and active noise control.
These projects involve the characterization of materials from the micron level down to atomic dimensions. The primary tools are electron microscopes (SEM and TEM). These unique instruments will not only allow students to image nanostructures and new materials but will allow them to probe structure, composition, and chemistry with high resolution.
We have a 16” remote telescope in central Utah operated both remotely over the internet via a satellite link and by on-0site personnel. This telescope is used to monitor variable objects such as pulsating stars and active galactic nuclei. Students can work on projects ranging from monitoring to image enhancement and analysis.
Constructing and characterizing a calcium beam source for an atomic clock. The beam will be generated by heating calcium atoms under high vacuum to produce a thermal vapor. A small hole in the oven will allow some of the vapor to spray out. The escaping vapor will be collimated by two very narrow slits. The student’s work would involve constructing the oven, measuring the velocity distribution and total flux of atoms using absorption spectroscopy, and comparing the measurements to theory to assure that the oven is operating properly.
There are a large number of astrophysical events that can be studied by finding and monitoring variable stars. My research program is currently working on methods of finding very low amplitude variables in open clusters. We find pulsating variable stars and eclipsing variable stars, and perhaps one day we will find an extra-solar planet. These stars give information about the clusters and the evolution of stars. In addition, we have been monitoring High-Mass X-ray Binary systems. This is a binary star system with one supermassive star in orbit around a black hole. We will likely monitor a number of these systems in the summer of 2008. REU students will work on a project in one of these fields by taking data either on campus, or at our West Mountain Observatory.
This research has been focused on studying the spin of electrons in semiconductors (spin is an inherent property of electrons, like charge or mass). We have been working on making experimental measurements of spin lifetimes in the semiconductor GaAs (gallium arsenide), its alloys, and in semiconductor nanostructures based on GaAs & alloys. Experimental techniques combine optical spectroscopies such as photoluminescence and reflectivity with magnetic resonance of the electron and nuclear spins. Experiments are done at very low temperatures (1.5 K) and large magnetic fields (1+ tesla). Students help in all aspects of the experimental work, including things like writing computer programs to control equipment and take data, aligning the lasers and optics, plotting and analyzing data, and filling up the magnet system with liquid helium.
Our research group is currently looking for both binary brown dwarf systems and binary objects in the Kuiper Belt using data from the Hubble Space Telescope (HST). An REU student would primarily work with us on refining the binary detection technique, looking for new binary systems, and characterizing the uncertainty in the detection approach and the final magnitudes, separations, etc. of the systems.
Radio-interferometry techniques is a powerful tool to study the processes involved in star formation and evolution.
The star formation process is shrouded in an environment of gas and dust which obscures the region and does not allow the study at optical frequencies. At the opposite end of star formation, Late-type Stars develop thick molecular shells which are also not detected in the visible spectrum. This leaves the radio regime of the electromagnetic spectrum as the most important window to study these processes. The high spatial resolution provided by the interferometric techniques used in arrays like the VLA and VLBA in the USA, MERLIN and ATCA in England and Australia, respectively, allow us to study the physical mechanisms by which stars are formed and later die.