Gas dynamics around a Jupiter mass planet: II. Chemical evolution of circumplanetary material
arXiv:2411.17408 · doi:10.1051/0004-6361/202451140
Abstract
In an ongoing effort to understand planet formation the link between the chemistry of the protoplanetary disk and the properties of resulting planets have long been a subject of interest. These connections have generally been made between mature planets and young protoplanetary disks through the carbon-to-oxygen (C/O) ratio. In a rare number of systems, young protoplanets have been found within their natal protoplanetary disks. These systems offer a unique opportunity to directly study the delivery of gas from the protoplanetary disk to the planet. In this work we post-process 3D numerical simulations of an embedded Jupiter-massed planet in its protoplanetary disk to explore the chemical evolution of gas as it flows from the disk to the planet. The relevant dust to this chemical evolution is assumed to be small, co-moving grains with a reduced dust-to-gas ratio indicative of the upper atmosphere of a protoplanetary disk. We find that as the gas enters deep into the planet's gravitational well, it warms significantly (up to K), releasing all of the volatile content from the ice phase. This change in phase can influence our understanding of the delivery of volatile species to the atmospheres of giant planets. The primary carbon, oxygen, and sulfur carrying ices: CO, HO, and HS are released into the gas phase and along with the warm gas temperatures near the embedded planets lead to the production of unique species like CS, SO, and SO compared to the protoplanetary disk. We compute the column densities of SO, SO, CS, and HCS in our model and find that their values are consistent with previous observational studies.
20 pages, 17 figures, accepted for publication in A&A
References in corpus (23)
- The NumPy array: a structure for efficient numerical computation
- The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package
- Gas- and dust evolution in protoplanetary disks
- Two accreting protoplanets around the young star PDS 70
- A comparative study of disc-planet interaction
- An Ice Age JWST inventory of dense molecular cloud ices
- A Circumplanetary Disk Around PDS70c
- Constraining the X-ray and Cosmic Ray Ionization Chemistry of the TW Hya Protoplanetary Disk: Evidence for a Sub-interstellar Cosmic Ray Rate
- Setting the volatile composition of (exo)planet-building material. Does chemical evolution in disk midplanes matter?
- Water in star-forming regions (WISH): Physics and chemistry from clouds to disks as probed by Herschel spectroscopy
- Reduced gas accretion on super-Earths and ice giants
- CO Depletion in Protoplanetary Disks: A Unified Picture Combining Physical Sequestration and Chemical Processing
- Formation of Giant Planet Satellites
- Connecting planet formation and astrochemistry: A main sequence for C/O in hot-exoplanetary atmospheres
- Evidence for a circumplanetary disk around protoplanet PDS 70 b
- Connecting planet formation and astrochemistry: Refractory carbon depletion leading to super-stellar C/O in giant planetary atmospheres
- Modeling accretion shocks at the disk-envelope interface -- Sulfur chemistry
- Tracing snowlines and C/O ratio in a planet-hosting disk: ALMA molecular line observations towards the HD169142 disk
- An upper limit on the mass of the circumplanetary disk for DH Tau b
- Hot Jupiter and ultra-cold Saturn formation in dense star clusters
- Chemical footprints of giant planet formation. Role of planet accretion in shaping the C/O ratio of protoplanetary disks
- ALMA high-resolution observations unveil planet formation shaping molecular emission in the PDS 70 disk
- Effective dust growth in laminar circumplanetary discs with magnetic wind-driven accretion