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A gas-grain time dependent chemical code, UCL\_CHEM, has been used toinvestigate the possibility of using chemical tracers to differentiate betweenthe possible formation mechanisms of brown dwarfs. In this work, we model theformation of a pre-brown dwarf core through turbulent fragmentation byfollowing the depth-dependent chemistry in a molecular cloud through the stepchange in density associated with an isothermal shock and the subsequentfreefall collapse once a bound core is produced. Trends in the fractionalabundance of molecules commonly observed in star forming cores are thenexplored to find a diagnostic for identifying brown dwarf mass cores formedthrough turbulence. We find that the cores produced by our models would bebright in CO and NH$_3$ but not in HCO$^+$. This differentiates them frommodels using purely freefall collapse as such models produce cores that wouldhave detectable transitions from all three molecules.

Chemical Tracers of Pre-Brown Dwarf Cores Formed Through Turbulent Fragmentation