Methanol Along the Path from Envelope to Protoplanetary Disc
Maria N. Drozdovskaya, Catherine Walsh, Ruud Visser, Daniel Harsono, and Ewine F. van Dishoeck

TL;DR
This study models the chemical evolution of interstellar methanol during star formation, revealing how infall paths affect methanol abundance in protoplanetary discs, with implications for organic molecule budgets in planetary systems.
Contribution
It introduces a 2D semi-analytic model combined with radiative transfer and chemical networks to trace methanol evolution from cloud to disc, considering different physical scenarios.
Findings
Infall path influences methanol abundance in discs.
Methanol is often reduced in the comet-forming zone compared to prestellar phase.
Physical conditions determine key chemical processes affecting methanol.
Abstract
Interstellar methanol is considered to be a parent species of larger, more complex organic molecules. A physicochemical simulation of infalling parcels of matter is performed for a low-mass star-forming system to trace the chemical evolution from cloud to disc. An axisymmetric 2D semi-analytic model generates the time-dependent density and velocity distributions, and full continuum radiative transfer is performed to calculate the dust temperature and the UV radiation field at each position as a function of time. A comprehensive gas-grain chemical network is employed to compute the chemical abundances along infall trajectories. Two physical scenarios are studied, one in which the dominant disc growth mechanism is viscous spreading, and another in which continuous infall of matter prevails. The results show that the infall path influences the abundance of methanol entering each type of…
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