Grimble, William; Kastner, Joel; Sargent, B.; Stassun, Keivan G. (2025).听.听Astrophysical Journal, 995(1), 86.听
To better understand聽protoplanetary disks鈥攖he disks of gas and dust around young stars where planets form鈥攕cientists need models that can explain both their聽spectra聽(how they emit light at different wavelengths) and their physical structure. In earlier work, the authors developed a combined approach called the聽EaRTH Disk Model, which links observational data from infrared spectra with聽radiative transfer models聽(simulations of how light moves through and interacts with matter).
In this study, they improve one part of that model: how temperature is distributed across the disk. Instead of using a more complex method that requires breaking the disk into many small pieces for calculation, they introduce a simpler mathematical description that still captures how temperature varies with location. This new approach uses an empirical (data-driven) relationship between spatial properties of the disk, making it easier for models to fit real observations while staying physically realistic.
They tested the updated model using infrared data from the聽Spitzer Space Telescope, focusing on聽transition disks聽(disks with gaps or holes that may indicate planet formation). The results provide insights into the disks鈥� composition (mineralogy) and structure, including evidence for聽grain growth and processing鈥攌ey steps in the early stages of planet formation.
Figure 1.聽Model fit plots of TZTD empirical mineralogical analysis of Spitzer/IRS spectra of targets indicated in Table聽. Red: cool-disk component constituents; blue: warm-disk component constituents; see Figure Set聽in the聽聽for legend of dust components.