I am also a member of the science team for the SPARCS cubesat led by PI Evgenya Shkolnik. SPARCS is a NASA funded 6U CubeSat dedicated to monitoring the high-energy radiation environment around low mass stars. Set to launch after October 2021, this one-year mission will measure short- and long-term variability of ~10 stars simultaneously in the far and near ultraviolet. My role on the team is to provide model spectra for these stars based on the SPARCS photometric measurements.
I am fifth year doctoral candidate studying planetary science at the University of Arizona's Lunar and Planetary Lab. I am interested in exoplanets and their atmospheres, specifically those around M dwarf stars. My research involves determining if a planet in the commonly-defined habitable zone is truly habitable by improving our understanding of the evolution of planetary atmospheres as they are subjected to large amounts of high energy radiation.
The chemistry and evolution of planetary atmospheres depends on the evolution of the high-energy radiation emitted by its host star. High levels of extreme ultraviolet (EUV) radiation can drastically alter planetary atmospheres through ionizing, heating, expanding, chemically modifying, and eroding them during the first few billion years of a planetary lifetime. Unfortunately, we are currently unable to observe in these wavelengths, but there are spectral observations of both shorter (x-ray) and longer (UV) wavelengths than the EUV. My research entails using the PHOENIX stellar atmosphere code to model the upper atmospheres of stars (where this energy comes from) in order to determine how much EUV radiation is emitted. Since we have x-ray and UV observations, I am able to constrain my models to the observed stellar spectra.
Currently, I am focusing on modeling M dwarf stars: stars that are smaller and cooler than the Sun. The reason for selecting these low-mass stars is that their low luminosities produce habitable zones much closer to the star (~0.1-0.4 AU), making it easier to find terrestrial (and potentially habitable!) planets around them.
Below is an example PHOENIX model spectrum (navy) of the M dwarf star, GJ176, as compared to the observed spectrum (red). The observed spectrum is from the MUSCLES HST Treasury Survey [France+ 2016; ApJ 820:89F]. The MUSCLES spectrum contains Chandra/XMM-Newton X-ray observations, empirically derived relations to compute the EUV spectrum, and observed HST COS and STIS spectra covering the Far-UV and Near-UV regions.
Art is rad.
The Art of Planetary Science is an annual art exhibit put on by the graduate students of LPL. I have had the pleasure of co-organizing the event for the past four years with the rest of the TAPS team: Jamie Molaro, James Keane, Hannah Tanquary, Theresa Hentz, and Tracy Esman.
This show acts as a way to bring together Tucson's art and astronomy communities through displays of art created from and inspired by the solar system and the scientific data with which we explore it. This past year, the show had over 200 submissions, with works from over 120 artists and scientists. Through this experience, we are able to connect with both the art community and over 1000 members of the public each year to share how planetary science is creative and beautiful.
Check out our website: www.lpl.arizona.edu/art for more information about the event.
My work with The Art of Plantery Science has inspired me to explore and play with different styles of art. Throughout the years I have created and exhibited pieces including yarn quipus counting various expolanet statistics, laser spirographs inspired by the ChemCam on the Curiosity rover, and an M dwarf stellar spectrum visualized as an aluminum windchime. In 2018 I started creating planetary science-inpsired acrylic pours: