Over the years, our research group has built two databases that will benefit the future planetary science and astronomy community.
A material property database for Titan-relevant organic liquids, ices, and solids: https://titanmaterials.sites.ucsc.edu/. The paper can be found here: doi.org/10.3847/1538-4365/acc6cf. The current version includes 18 simple organic species that are detected on Titan: CH4, C2H6, C2H4, C2H2, C4H2, C6H6, C3H8, C3H6, C3H4-a (allene), C3H4-p (propyne), HCN, HC3N, CO2, CH3CN, C2H5CN, C2H3CN, C2N2, C4N2 and the measured properties of Titan haze analogs (“tholins”) from 6 laboratories. We summarize and compute the following properties in the current released version: thermodynamic properties (phase change points, sublimation saturation vapor pressure (sublimation SVP), vaporization saturation vapor pressure (vaporization SVP), and sublimation and vaporization latent heat), physical properties (organic liquid density, organic ice density, and haze density), and surface properties (organic liquid surface tension, organic ice surface energy, and haze surface energy). We envision these data to be useful for modeling/observational data analysis efforts on Titan. Beyond Titan, the material properties of the simple organics may also be applicable for giant planets and icy bodies in the outer solar system, interstellar medium, protoplanetary disks, and exoplanets.
A hazy exoplanet property database: https://exoplanethaziness.shinyapps.io/hazyweb/. The current version includes the properties of 25 cool exoplanets (equilibrium temperature < 1000 K) that have been observed with the Wide Field Camera Three of the Hubble Space Telescope. The paper can be found here: doi.org/10.3847/1538-4357/ac7f40. These planets provide key insights into our understanding of photochemical hazes in planetary atmospheres. The database summarizes a range of planetary properties and stellar properties of each planet. It also calculates a haziness metric we developed (called “water amplitude”) to quantify how hazy an exoplanet is. It allows users to freely plot the relationship between the haze metric and any stellar/planetary parameters and statistics values are automatically computed for each plot. Any statistical trend that exists between a parameter and the haze metric would help us identify key processes that control haze formation on exoplanets. As the field evolves with more upcoming spectroscopic observations of exoplanets, we will keep updating the database with new observations and keep track of any updated trends.