Journey of complex organic molecules: Formation and transport in protoplanetary disks

¹ Aix-Marseille Université, CNRS, CNES, Institut Origines, LAM, Marseille, France
² Institut Universitaire de France (IUF), Paris, France
³ Aix-Marseille Université, CNRS, Institut Origines, PIIM, Marseille, France
⁴ Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA, USA

^★ Corresponding author; tommy.benest@gmail.com

Received: 5 February 2024
Accepted: 16 October 2024

Abstract

Context. 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.

Aims. 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.

Methods. 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.

Results. On average, particles ranging from 1 to 100 µm 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 µm in size, released at a local temperature of 80 K, receive sufficient irradiation after 141 and 359 kyr. In contrast, 1 cm sized particles would require several million years to receive this level of irradiation, which is infeasible since they cross the iceline within approximately 500 kyr.

Conclusions. 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.