I compared synthetic spectra from simulated convective hydrodynamic (HD) flows to convective magnetohydrodynamic (MHD) flows to analyze the effects of magnetic fields on the chemical abundance in the solar photosphere. I compared a local dynamo simulation (0 net vertical magnetic flux) to a mean field (non-zero constant magnetic flux) magnetic simulation to uncover unique signatures in the spectral line shapes. I deduced the two magnetic field morpholoogies' influence on oxygen and iron abundances from visible spectral line diagnostics. This research is published in Moore, C. S. et al., 2015, The Effects of Magnetic Field Morphology on the Determination of Oxygen and Iron Abundances in the Solar Photosphere, ApJ, 799 150. 

I worked with Dr. James Chervenak and Dr. Thomas Stevenson in the Detector System Branch, Code 553, to learn the fundamentals of solid state physics, electronics and clean room processes to develop microstructure devices. My projects were to: 1. Create a terahertz (far-infrared) emitter that will operate between 4 and 20 K and calibrate a detector and 2. Test the effects of a new deposition mechanism (Plasma Enhanced Chemical Vapor Deposition) of silicon oxide SiO2 insulating layers on the critical current (maximum current a superconductor can maintain) of niobium. These devices are micro meter size (smaller than the width of your hair), so it is necessary to build them in an environment where there are few large particles, called a “clean room”. I received training on high temperature furnaces, photolithography, implantation of dopant ions, electron-beam deposition of metals, dry and wet etching and microscope usage. This experience bestowed upon me critical insight on connecting science and engineering. 

I worked with Dr. Brian Dennis in the Solar Physics Branch, Code 671, and learned how to analyze X-Ray spectra and images from the Ramaty High Energy Solar Spectroscopic Imager (RHESSI). RHESSI is a solar X-ray imaging spacecraft with spectroscopic capabilities. I utilized IDL to analyze spectra for 30 + solar flares from the last sunspot solar cycle. I deduced the energy budgets for the accelerated electrons and the thermal plasma by fitting curves of count rate versus photon energy to physical models. The results from my first three internships are published in Emslie, A. G., Chamberlin, P. C., Dennis, B. R., Mewaldt, R. A., Moore, C. S. , Share, G. H., Shih, A. Y, Vourlidas, A. and Welsch, B. T., 2012, Global Energetics of Thirty-Eight Large Solar Eruptive Events, ApJ, 759 71. During this work, Dr. Dennis provided guidance on RHESSI spacecraft design, data acquisition and data processing.

I worked with Dr. Phillip Chamberlin and Dr. Rachel Hock analyzing data from the Total Irradiance Monitor (TIM) which flies onboard NASA‘s SOlar Radiation and Climate Experiment (SORCE) mission. The first research objective was to deduce the total amount of energy released from X-class (the most energetic) solar flares across the entire electromagnetic spectrum. Solar flares are eruptions of material confined by twisted magnetic field lines. Another objective was to obtain the contribution from the vacuum ultraviolet (VUV) wavelengths with the help of the Flare Irradiance Spectral Model (FISM). I used this model to decompose the solar flares into their impulsive and gradual phases. During my internship I learned the computer program Interactive Data Language (IDL). I compared FISM models of irradiance versus time to data from TIM to put constraints on the energy fluctuations in the Total Solar Irradiance due to solar flares. The results of this study are published in Moore, C. S., Chamberlin, P. C. and Hock, R., 2014, Measurements and Modeling of Total Solar Irradiance in X-class Solar Flares, ApJ, 787 32M. This experience taught me computer programming skills and the basics of analyzing data from space based facilities.