Stellar Astrophysics

Caty Pilachowski

Caty PilachowskiCatherine Pilachowski’s research on stellar astrophysics focuses on abundances of the odd light elements such as fluorine, chlorine, and phosphorus to contribute to our general understanding of chemical evolution and the origin of elements.

The odd light elements are particularly interesting because their origins are not well understood Prior to a few years ago, little was known about their abundances in stars. Determining the abundances of these elements is challenging, since their spectral features like mostly in the infrared. These elements are formed through unusual channels of nucleosynthesis. Possible mechanisms to make F, Cl, and P include mixing during hydrostatic burning stages in massive stars, decay from heavier radioactive isotopes formed during explosive nucleosynthesis, and even neutrino spallation during Type II supernovae explosions. The abundances of these elements may thus provide clues to nuclear reactions in extreme environments.

Katherine Rhode

Kathy Rhode

Katherine Rhode’s research interests include the evolution of young, Sun-like stars and their surrounding protoplanetary disks. She and her students use the Hydra multi-fiber spectrograph on the WIYN 3.5-m telescope to measure the rotational velocities and sizes of young stars in nearby star clusters like the Orion Nebula Cluster, IC 348, and NGC 2264 (a.k.a. the Christmas Tree Cluster). These young stars are in the early stages of forming their own planetary systems, so studying how the stars evolve and interact with their protoplanetary disks helps us better understand the origins of our own Solar System.

Songhu Wang

Songhu WangSonghu Wang’s research on stellar astrophysics centers on understanding exoplanet host stars, which will help him better characterize the structure and composition of exoplanets they host.

Wang uses high-resolution spectra collected with NEID to measure stellar atmospheric parameters. Combined with distance measurements from GAIA, these parameters will provide us with precise size and mass measurements of exoplanetary host stars. Knowing the sizes and masses of stars lets us precisely measure the sizes and masses of planets.

Using high-resolution spectra from NEID, we can also measure exoplanetary host stars’ projected rotation velocity (vsini). Combining vsini measurements with stellar rotation period measurements from TESS, we can investigate the obliquity distribution of exoplanetary host stars, which will provide us with critical information on the formation history of exoplanets.