I am a Research Space Scientist in the Planetary Environments Laboratory (Code 699), part of the Solar System Exploration Division (Code 690) at NASA Goddard Space Flight Center. Previously, I was a Postdoctoral Fellow of the NASA Postdoctoral Program in the Planetary Systems Laboratory (Code 693) at Goddard Space Flight Center, working with Dr. Geronimo Villanueva.
I am interested broadly in planetary atmospheres, more specifically in aeronomy and atmospheric chemistry. My current research is focused on the atmosphere of Mars and uses data collected by the Neutral Gas and Ion Mass Spectrometer (NGIMS) onboard the NASA Mars Atmosphere and Volatile EvolutioN (MAVEN) mission and the Nadir and Occultation for MArs Discovery (NOMAD) insrument on the ESA ExoMars Trace Gas Orbiter (TGO). Scroll down to the Research section to read more.
I received a Doctorate and Master of Science in Planetary Sciences from the Lunar and Planetary Laboratory at the University of Arizona, where my advisor was Prof. Roger V. Yelle; a Master of Science in Organic Chemistry from the University of California, Los Angeles, while working in the lab of Prof. Timothy J. Deming, where I synthesized polypeptides developed as biomolecular materials for, e.g., drug delivery; and a Bachelor of Science in Chemistry from the University of Texas at Dallas, where I synthesized organic polymers for, fabricated, and tested polymer solar cells with Prof. John P. Ferraris.
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We use MAVEN NGIMS data to investigate the composition of the Martian upper atmosphere, focusing on the variations of CO2, Ar, N2, O, He, and H2 with Martian local time, latitude, season, and temperature. We find large diurnal variations in the abundances of the lighter species: N2, O, He, and H2. Our measurements are the first vertical profiles and the first spatially- and temporally-resolved measurements of the H2 abundance on Mars.
We discovered substantial amounts of H2O in the upper atmosphere of Mars, around 150 km above the surface, throughout the Martian year. The upper atmospheric water abundance peaks when Mars is closest to the Sun during summer in its southern hemisphere. Martian dust storms, including the 2018 global storm which put the Opportunity rover out of commission, are a sudden splash of water into the upper atmosphere. The classical process for delivery of hydrogen, in contrast, delivers a steady trickle of hydrogen to the upper atmosphere in the form of H2.
We derive neutral temperatures from Ar, CO2, and N2 abundances measured by MAVEN NGIMS over 1.5 Martian years. The temperature profiles cover an altitude range of 150 to roughly 300 km on nominal orbits. During Deep Dips, temperature profiles extend down to about 125 km, near the mesopause. We characterize thermospheric gradients and exospheric temperatures. The thermal structure of the Martian upper atmosphere is important for quantifying loss of the atmosphere to space.
Upcoming and past talks and posters.
I gave a talk entitled, "Isotope Ratios in the Martian Upper Atmosphere Measured by MAVEN NGIMS" at the 2022 annual meeting of the American Astronomical Society Division for Planetary Sciences in London, Ontario.
I gave a talk entitled, "Isotope Ratios in the Martian Upper Atmosphere Measured by MAVEN NGIMS" at the 2022 Europlanet Science Congress hosted by the Europlanet Society in Granada, Spain.
I gave a talk entitled, "Transport and Escape of Water: Toward a More Complete Interpretation with TGO NOMAD and MAVEN NGIMS" at the seventh Mars Atmosphere Modeling and Observations workshop in at Sorbonne University in Paris, France.
I presented a poster entitled, "Isotope Ratios in the Upper Atmosphere of Mars from MAVEN NGIMS" at Mars Workshop V, which was held at the Les Houches School of Physics in Les Houches, France. Click the button below to see this research in slide form.