Hello, I’m Jiayin Dong. I’m a 4th-year graduate student at Penn State Department of Astronomy & Astrophysics, where my advisor is Bekki Dawson. I’m broadly interested in exoplanets and planet(-ary system) formation and evolution. I was previously a predoctoral fellow at CCA, Flatiron Institute where I worked with Phil Armitage and Yan-Fei Jiang.
Interests. Exoplanets, Debris disks, Planet formation, N-body simulations, Hydrodynamic simulations, Probabilistic data analysis
A Catalog of Warm, Large Exoplanets Discovered in Year 1 TESS Full-Frame Images
Warm, Large Exoplanets (WaLEs) are a key missing piece in our understanding of how planetary systems form and evolve. It is currently debated whether WaLEs form in situ, undergo disk or high eccentricity tidal migration, or have a mixture of origin channels. These different classes of origin channels lead to different expectations for WaLEs’ properties, e.g., their eccentricities and companion properties, which are currently difficult to examine due to the small WaLE sample size. In this project, we uniformly search for WaLE candidates around main-sequence host stars brighter than TESS-band magnitude of 12 in southern ecliptic hemisphere in Year 1 TESS Full-Frame Images. We introduce a catalog of WaLE candidates and charaterize their eccentricities, transit-timing variations (TTVs), and the eccentricity distribution.
Terminal Rotation Rates of Gas Giants in the Unmagnetized Limit
Planetary spin is the fingerprint of planet formation. In the absence of planetary winds or strong tidal effects, planetary rotation is expected to remain almost unchanged since the end of planet formation, providing direct evidence by which we can compare theoretical models of giant planet formation against observations. In this work, we explore one perspective of planetary spin evolution: the spin up of the protoplanet through its circumplanetary disk (CPD). We ask what is the terminal rotation rate of gas giant planets in the unmagnetized limit? The answer is not the breakup velocity as normally expected, but depends on the CPD scale height.
Debris Disks in Multiplanet Systems: Are Our Inferences Compromised by Unseen Planets?
Debris disks features (e.g., warps, offsets, edges and gaps, azimuthal asymmetries, thickened rings, scale heights) have often been recognized as the signposts of planets. Most existing models assume a single planet is sculpting the disk feature, but recent observations of mature planetary systems have revealed that many planets reside in multi-planet systems. In this work, we investigate if/how planet properties inferred from single-planet models are compromised when multiple planets reside in the system.