3:45 PM - 4:00 PM
[PPS06-08] Model calculation of infrared and radio observations of the circumplanetary disks: Conditions for satellite formation
Keywords:circumplanetary disk, radiative transfer calculation, infrared observations, radio observations
Satellites are believed to be formed from circumplanetary disks. There are various theoretical models of satellite formation, but there are few observational constraints on the physical quantity of the circumplanetary disks. It is known that the ice-rock ratio of Jupiter's moons are not uniform. In the hot regions inside the water snow line in the circumplanetary disks, ice vaporizes and rocks become the main material for satellites. Therefore, it is important to investigate the physical quantity of the circumplanetary disks, especially the temperature, when considering the conditions for satellite formation. In recent years, detailed structures of protoplanetary disks around many young stars have been observed using high-resolution ALMA telescopes. In addition, structures similar to the circumplanetary disks were discovered. It is also expected that the infrared space telescope JWST, which is scheduled to be launched in 2021, will detect more circumplanetary disks.
In this study, we aim to establish a method for investigating the temperature of the circumplanetary disks by comparing model calculations with these observations. Previous studies have predicted the intensities of the dust and gas emission at (sub)millimeter wavelengths of the turbulent viscous accretion disks (Zhu et al. 2018) and the irradiation heating disks (Rab et al. 2019), for ALMA observations. In this study, we perform model calculations of dust and gas emission from circumplanetary disks, using the viscous accretion disk model, for JWST observations, and investigate how the intensities change for the models with different physical quantities, such as the accretion rate and the viscous parameter, alpha. As a result, it was shown that the circumplanetary disks is detectable relatively easily with dust continuum emission by JWST. Furthermore, chemical reaction calculations were performed to predict the intensities of various molecular lines and investigate how the infrared and (sub)millimeter line intensities depend on the physical quantity of the disk, and their detectabilities were also investigated.
In this study, we aim to establish a method for investigating the temperature of the circumplanetary disks by comparing model calculations with these observations. Previous studies have predicted the intensities of the dust and gas emission at (sub)millimeter wavelengths of the turbulent viscous accretion disks (Zhu et al. 2018) and the irradiation heating disks (Rab et al. 2019), for ALMA observations. In this study, we perform model calculations of dust and gas emission from circumplanetary disks, using the viscous accretion disk model, for JWST observations, and investigate how the intensities change for the models with different physical quantities, such as the accretion rate and the viscous parameter, alpha. As a result, it was shown that the circumplanetary disks is detectable relatively easily with dust continuum emission by JWST. Furthermore, chemical reaction calculations were performed to predict the intensities of various molecular lines and investigate how the infrared and (sub)millimeter line intensities depend on the physical quantity of the disk, and their detectabilities were also investigated.