Journey of complex organic molecules: Formation and transport in protoplanetary disks
arXiv:2412.09271 · doi:10.1051/0004-6361/202449499
Abstract
Complex organic molecules serve as indicators of molecular diversity. Their detection on comets, planets, and moons has prompted inquiries into their origins, particularly the conditions conducive to their formation. One hypothesis suggests that the UV irradiation of icy grains in the protosolar nebula generates significant molecular complexity, a hypothesis supported by experiments on methanol ice irradiation. We investigated the irradiation of methanol ice particles as they migrate through the protosolar nebula. Our objective is to ascertain whether the encountered conditions facilitate the formation of complex organics molecules, and we leverage experimental data in our analysis. We developed a two-dimensional model that describes the transport of pebbles during the evolution of the protosolar nebula, employing a Lagrangian scheme. This model computes the interstellar UV flux received by the particles along their paths, which we compared with experimental values. On average, particles ranging from 1 to 100 micrometers in size, released at a local temperature of 20 K, undergo adequate irradiation to attain the same molecular diversity as methanol ice during the experiments within timescales of 25 kyr of protosolar nebula evolution. In contrast, 1 cm sized particles require 911 kyr of irradiation to reach similar molecular diversity, making comparable molecular complexity unlikely. Similarly, particles ranging from 1 to 100 micrometers in size, released at a local temperature of 80 K, receive sufficient irradiation after 141 and 359 kyr. The particles readily receive the irradiation dose necessary to generate the molecular diversity observed in the experiments within the outer regions of the disk. Our model, combined with future irradiation experiments, can provide additional insights into the specific regions where the building blocks of planets form.
arXiv comment12 pages, 7 figures. Published in A&A
References in corpus (28)
- Observations of the Icy Universe
- Using FU Orionis Outbursts to Constrain Self-Regulated Protostellar Disk Models
- A simple model for the evolution of the dust population in protoplanetary disks
- Formation rates of complex organics in UV irradiated CH3OH-rich ices I: Experiments
- Photochemistry and astrochemistry: photochemical pathways to interstellar complex organic molecules
- Radial Flow of Dust Particles in Accretion Disks
- The Disk Substructures at High Angular Resolution Project (DSHARP): V. Interpreting ALMA maps of protoplanetary disks in terms of a dust model
- Testing grain-surface chemistry in massive hot-core regions
- Evolution of protoplanetary disks: Constraints from DM Tauri and GM Aurigae
- ISO spectroscopy of gas and dust: from molecular clouds to protoplanetary disks
- Increased complexity in interstellar chemistry: Detection and chemical modeling of ethyl formate and n-propyl cyanide in Sgr B2(N)
- Early Evolution of Stellar Groups and Clusters: Environmental Effects on Forming Planetary Systems
- Astrochemistry of dust, ice and gas: introduction and overview
- Detection of abundant solid methanol toward young low mass stars
- An experimental study of the surface formation of methane in interstellar molecular clouds
- Residence Times of Particles in Diffusive Protoplanetary Disk Environments I. Vertical Motions
- Residence Times of Particles in Diffusive Protoplanetary Disk Environments II. Radial Motions and Applications to Dust Annealing
- Hydrogenation of accreting C-atoms and CO molecules -- simulating ketene and acetaldehyde formation under dark and translucent cloud conditions
- Rocklines as Cradles for Refractory Solids in the Protosolar Nebula
- Formulas for Radial Transport in Protoplanetary Disks
- Pebble accretion at the origin of water in Europa
- Jupiter's "Cold" Formation in the Protosolar Disk Shadow: An Explanation for the Planet's Uniformly Enriched Atmosphere
- Sticky or not sticky? Measurements of the tensile strength of micro-granular organic materials
- Rocky Planetesimal Formation Aided by Organics
- Evolution of the reservoirs of volatiles in the protosolar nebula
- Tracking Dust Grains During Transport and Growth in Protoplanetary Disks
- Synthesis of molecular oxygen via irradiation of ice grains in the protosolar nebula
- Monte Carlo Simulation of Sugar Synthesis on Icy Dust Particles Intermittently Irradiated by UV in a Protoplanetary Disk