A Framework for Characterizing Transmission Spectra of Exoplanets with Circumplanetary Rings

TL;DR

This paper introduces a framework to analyze how circumplanetary rings influence exoplanet transmission spectra, helping distinguish ring effects from atmospheric aerosols in featureless spectra.

Contribution

It develops an analytical model and a post-processing method to incorporate rings into transmission spectra, advancing understanding of their spectral signatures and stability conditions.

Findings

Rings can flatten transmission spectra across viewing angles.

Future JWST observations can differentiate rings from aerosols.

Rocky rings may produce a detectable silicate feature at 10 μm.

Abstract

Recent observations revealed that several extremely low-density exoplanets show featureless transmission spectra. While atmospheric aerosols are a promising explanation for both the low density and featureless spectra, there is another attractive possibility: the presence of circumplanetary rings. Previous studies suggested that rings cause anomalously large transit radii. However, it remains poorly understood how rings affect the transmission spectrum. Here, we provide a framework to characterize the transmission spectra of ringed exoplanets. We develop an analytical prescription to include rings in the transmission spectra for arbitrarily viewing geometries. We also establish a simple post-processing model that can include the ring's effects on precomputed ring-free spectra. The ring flattens the transmission spectrum for a wide range of viewing geometries, consistent with the featureless spectra of extremely low-density exoplanets. Near-future observations by JWST at longer wavelengths would be able to distinguish the aerosol and ring scenarios. We also find that rocky rings might cause a silicate feature at $\sim$10 $\mu$m if the ring's optical depth is around unity. Thus, the ring's spectral features, if detected, would provide tight constrains on the physical properties of exoplanetary rings. We also discuss the ring's stability and suggest that thick rings are sustainable only at the equilibrium temperature of $\lesssim$300 K for the ring's age comparable to Kepler planets. This might indicate the intrinsic deficit of thick rings in the Kepler samples, unless rings are much younger than the planets as suggested for Saturn.