The evolution of complex organic molecules during star formation

Complex organic molecules (COMs) are thought to be the precursors of pre-biotic molecules and are observed in many protostellar sources. For this paper we studied the formation of COMs during star formation and their evolution in the midplane of the circumstellar disk up to the end of the Class I stage. We used the Analytical Protostellar Environment (APE) code to perform analytical simulations of star formation and the Nautilus code to model the chemical evolution. Most COMs mainly form during the collapse or in the disk, except the lightest (CH 3 CCH, C 3 H 6 , CH 3 OH, CH 3 CHO, CH 3 OCH 3 , C 2 H 5 OH, CH 3 CN, CH 3 NC, C 2 H 3 CN, and CH 3 SH), which are significantly inherited by the disk from the prestellar phase. Over the first 150 kyr of the disk, the abundances of several COMs in the midplane vary negligibly (e.g., CH 3 CCH, CH 3 OH, and CH 3 CN), while others experience a variation of one order of magnitude (e.g., C 2 H 3 CHO HOCH 2 CHO, and CH 3 COCH 2 OH). Changing physical conditions also have an impact on the abundance profiles of COMs in the disk, and their inheritance. For example, increasing the temperature of the molecular cloud from 10 K to 15 K significantly promotes the formation of COMs in the prestellar phase, notably c-C 2 H 4 O and N-bearing species. Conversely, increasing the cloud mass from 2 M ⊙ to 5 M ⊙ only has a minor effect on the disk abundances in the early stages.