In my research I measure the fundamental properties of stars using some of the most powerful techniques of modern stellar astrophyiscs, such as asteroseismology and interferometry. By measuring stellar properties such as mass, radius, temperature, and age with greater precision and accuracy, we are able to test and improve our models of stellar structure and evolution, and learn about the population of stars in our galaxy, and subsequently their planets.

I am particularly interested in measuring the properties of the brightest stars in the sky. These stars have a rich history of observation, and are often readily amenable to follow-up observations. Sometimes, however, they can be difficult to study. This is because many modern instruments are designed to observe faint objects, so these bright stars saturate detectors, making calibrating and analysing observations of these stars challenging. This is the case for photometric observations made with the NASA space telescopes Kepler and TESS that we use to measure stellar oscillations. I have developed a series of Python packages to overcome these challenges. More information about these packages can be found on my Research page, and the repositories found at my github page.