Delivery of complex organic molecules to the system of Jupiter

Abstract

Complex organic molecules are key markers of molecular diversity, and their formation conditions in protoplanetary disks remain an active area of research. These molecules have been detected on a variety of celestial bodies, including icy moons, and may play a crucial role in shaping the current composition of the Galilean moons. Experimental studies suggest that their formation could result from UV irradiation or thermal processing of NH3:CO2 ices. In this context, we investigate the formation of complex organic molecules in the protosolar nebula and their subsequent transport to the Jupiter system region. Lagrangian transport and irradiation simulations of 500 individual particles are performed using a two-dimensional disk evolution model. Based on experiments with UV irradiation and thermal processing of CO2:NH3 ice, this model allows us to estimate the estimate the potential for the formation of complex organic molecules through these processes. Almost none of the particles released at a local temperature of 20 K (corresponding to ~12 AU from the Sun) reach the location of the system of Jupiter. However, when released at a local temperature of 80 K (~7 AU), approximately 45% of the centimetric particles and 30% of the micrometric particles can form complex organic molecules via thermal processing, subsequently reaching the location of the system of Jupiter within 300 kyr. Assuming that the Galilean moons formed in a cold circumplanetary disk around Jupiter, the nitrogen-bearing species potentially present in their interiors could have originated from the formation of complex organic molecules in the protosolar nebula.

10 pages, 5 figures

References in corpus (20)

• Coagulation, fragmentation and radial motion of solid particles in protoplanetary disks
• Testing grain-surface chemistry in massive hot-core regions
• The distribution of CO${}_2$ on Europa indicates an internal source of carbon
• Evidence for a circumplanetary disk around protoplanet PDS 70 b
• Formation of moon systems around giant planets: Capture and ablation of planetesimals as foundation for a pebble accretion scenario
• Meridional Circulation of Dust and Gas in the Circumstellar Disk: Delivery of Solids onto the Circumplanetary Region
• Rocklines as Cradles for Refractory Solids in the Protosolar Nebula
• Pebble accretion at the origin of water in Europa
• Constraints from deuterium on the formation of icy bodies in the Jovian system and beyond
• UV photoprocessing of NH3 ice: photon-induced desorption mechanisms
• Evolution of the reservoirs of volatiles in the protosolar nebula
• Early stages of Galilean moon formation in a water-depleted environment
• Tracking Dust Grains During Transport and Growth in Protoplanetary Disks
• Circumplanetary disk ices. I. Ice formation vs. viscous evolution and grain drift
• Deuterated water ice on the satellites of Saturn
• Monte Carlo Simulation of Sugar Synthesis on Icy Dust Particles Intermittently Irradiated by UV in a Protoplanetary Disk
• Effects from different grades of stickiness between icy and silicate particles on carbon depletion in protoplanetary disks
• Circumplanetary disk ices II. Composition
• The role of ammonia in the distribution of volatiles in the primordial hydrosphere of Europa
• Journey of complex organic molecules: Formation and transport in protoplanetary disks