Increasing the strength of the interstellar radiation field or theĬosmic-ray ionization rate with respect to the typical values assumed in nearby Overlaps with the dust continuum, consistent with the observed chemical Extended methanol emission is shifted towards colderĪnd more shielded regions of the core envelope while $c$-C$_3$H$_2$ emission Model is able to reproduce several aspects of the observed chemicalĭifferentiation in L1544. Observed chemical segregation in the prototypical pre-stellar core L1544. Observations to determine which initial conditions are compatible with the
Nine different chemical models are compared to the Results are analyzed and compared to observations of CH$_3$OHĪnd $c$-C$_3$H$_2$ in L1544. A 3D MHD model of a pre-stellar coreĮmbedded in a dynamic star-forming cloud is post-processed using sequentiallyĬontinuum radiative transfer, a gas-grain chemical model, and a line-radiative Of these cores we can establish the initial conditions for star and planetįormation and determine to what degree the chemical composition of pre-stellarĬores is inherited to the later stages. By characterizing the physical and chemical structure Jensen and 4 other authors Download PDF Abstract: Pre-stellar cores represent the earliest stage of the star- and Environmental and structural impact on the distribution of CH$_3$OH and $c$-C$_3$H$_2$, by S. Download a PDF of the paper titled A 3D physico-chemical model of a pre-stellar core.
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