Research

Interests

Gallery of disk images from the DSHARP ALMA Large Program

Observational signatures of planet-disk interactions

Where, when, and how do planets form? Protoplanets are generally not expected to be massive enough to image directly, but their gravitational influence can carve rings, spirals, and asymmetries in protoplanetary disks. Our ALMA observations, most notably from the DSHARP Large Program, have shown that complex structures are common in disks, but exhibit a wide range of properties. The widespread presence of gap and ring structures suggest that giant planet formation can occur rapidly (within a million years or so) at distances even past a hundred au from the star.

Environmental influences on planet formation

Our understanding of disk structure and evolution has been in large part shaped by observations of relatively isolated disks in the closest star-forming regions. Our molecular line and scattered light observations, though, are increasingly uncovering evidence that protoplanetary disks are often dynamically perturbed by processes such as late infall and stellar encounters. In addition, we are studying the properties of disks in more distant star-forming regions that are exposed to more extreme levels of radiation compared to the commonly studied nearby disks.

Chemical diversity in the era of planet formation

Our observations have shown that disk rings and gaps are common not just in dust emission, but also in many molecular species. In some cases these molecular gaps and rings are likely the direct consequence of planet-disk interactions, much like the dust gaps and rings. In other cases, they are a consequence of disk chemistry. In addition, we also find marked chemical differences between disks. We seek to understand how these chemical differences may be tied to the disk structure, age, and environment.

Publications

Links to publications can be found here.