1D accretion discs around eccentric planets: observable near-infrared variability

Abstract

I present the results of 1D models of circumplanetary discs around planets on eccentric orbits. I use a classical viscous heating model to calculate emission fluxes at the wavelengths targeted by the NIRCam instrument on JWST, and compare the variability of this signal with the published NIRCam sensitivity specifications. This variability is theoretically detectable by JWST for a sufficiently viscous disc ($\alpha \sim 10^{-2}$) around a sufficiently eccentric planet ($e\sim 0.1-0.2$) and if the circumplanetary disc accretes material from its parent disc at a rate $\dot{M}\gtrsim 10^{-7}{\mathrm{M}}_{\odot }{\mathrm{yr}}^{-1}$. I discuss the limitations of the models used, and the implications of the result for probing the effectiveness of disc interactions for growing a planet's orbital eccentricity.

5 pages, 4 figures, submitted to MNRAS; replaced with version accepted for publication

References in corpus (5)

• Accreting Circumplanetary Disks: Observational Signatures
• The Hot Inner Disk of FU Ori
• Gas accretion onto planetary cores: three-dimensional self-gravitating radiation hydrodynamical calculations
• Young Stellar Object Variability (YSOVAR): Long Timescale Variations in the Mid-Infrared
• Searching for circumplanetary disks around LkCa 15

Cited by in corpus (1)

• Effects of the Planetary Temperature on the Circumplanetary Disk and on the Gap