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I am interested in characterizing the physical processes that shape protoplanetary disks to better understand how the current exoplanet population, and our own solar system, came to be. I primarily use ALMA to study line-emission from resolved disks, which allows me to interpret kinematic signatures, 2-D structure, and the chemical composition of these disks. These observations allow us to better understand planet formation, molecular emission surfaces, thermal structure, disk winds, turbulence, and more.
A Streamer Driving Misalignment in the Circumtriple Disk of GW Ori
GW Ori is a triple stellar system with a disk featuring three misaligned dust rings. This work presents ALMA molecular line data of CO isotopologues, revealing a streamer feeding the disk. Our results suggest that GW Ori remains dynamically linked to its parental cloud through ongoing accretion, with the streamer serving as the likely driver of its misaligned disk structure.
Late-Stage Infall
Late-Stage Infall
exoALMA
exoALMA
exoALMA V: Gaseous Emission Surfaces and Temperature Profiles
I am part of the exoALMA collaboration, an ALMA large program focused on detecting still-forming exoplanets. My work focuses on the gaseous emission surfaces and temperature structures of the fifteen protoplanetary disks covered by this program.
Winds Shape Planet Formation
Winds Shape Planet Formation
MAPS: Complex Kinematics in the AS 209 Disk Induced by a Forming Planet and Disk Winds
A kinematic analysis of the AS209 disk revealed strong winds in the vertical direction, coinciding with a gap seen in 12CO. These winds, likely launched by magnetohyrdodynamic (MHD) effects, may have a direct impact on the still-forming planet detected within the disk (AS209-b).
The Chemistry of Star Formation
The Chemistry of Star Formation
A Survey of Deuterated Ammonia in the Cepheus Star-Forming Region L1251
While at the University of Arizona I worked on understanding early star formation with Dr. Yancy Shirley. Cepheus L1251 is a nearby star forming region with several dense cores that will one day fully collapse to become stars. In the meantime, studying the chemistry within those cores can tell us about the chemical and kinematic evolution of star formation. Using the 12-meter telescope on Kitt Peak, I took observations of the 22 dense-cores to detect deuterated ammonia (o-NH2D). We detected o-NH2D in 13 of the 22 cores, which deepened our understanding of their evolution.
Observations of a 6' by 6' region in Cepheus L1251 with the 12-meter ARO telescope with two dense cores visible.
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