Abstract:In the interstellar medium (ISM), the formation of complex organic molecules (COMs) is largely facilitated by surface reactions. However, in cold dark clouds, thermal desorption of COMs is inefficient because of the lack of thermal energy to overcome binding energies to the grain surface. Non-thermal desorption methods are therefore important explanations for the gas-phase detection of many COMs that are primarily formed on grains. Here we present a new non-thermal desorption process: cosmic ray sputtering of … Show more
“…One possibility is low-temperature sputtering of CH 3 OH off grains by, for example, CO 2 , models of which reproduced observed gas-phase CH 3 OH abundances in Taurus Molecular Cloud within a factor of 2.5. 48 In addition, grain–grain collisions resulting from turbulence have been offered as an explanation for gas-phase organics in cold regions. 49 X-ray photodesorption of CH 3 OH at 15 K in disks has also been demonstrated experimentally.…”
Much of what is known about chemistry in star-forming regions comes from observations of nearby (d ∼ < 500 pc) low-mass protostars. For chemistry in high-mass star-forming regions, several more...
“…One possibility is low-temperature sputtering of CH 3 OH off grains by, for example, CO 2 , models of which reproduced observed gas-phase CH 3 OH abundances in Taurus Molecular Cloud within a factor of 2.5. 48 In addition, grain–grain collisions resulting from turbulence have been offered as an explanation for gas-phase organics in cold regions. 49 X-ray photodesorption of CH 3 OH at 15 K in disks has also been demonstrated experimentally.…”
Much of what is known about chemistry in star-forming regions comes from observations of nearby (d ∼ < 500 pc) low-mass protostars. For chemistry in high-mass star-forming regions, several more...
“…Species such as ions and radicals resulting from UV absorption that remain in the grain mantle can react further to form more complex species. Sputtering by strong jets and shock emission knots can spot raise the grain temperature and inject frozen intact methanol into the gas-phase (e.g., Draine 1995, Wakelam et al 2021, Paulive et al 2022).…”
We present results from the first molecular line survey to search for the fundamental complex organic molecule, methanol (CH3OH), in 14 Class 0/I proto-brown dwarfs (proto-BDs). IRAM 30-m observations over the frequency range of 92-116 GHz and 213-280 GHz have revealed emission in 14 CH3OH transition lines, at upper state energy level, Eupper ∼7-49 K, and critical densities, ncrit of 105 to 109 cm−3. The most commonly detected lines are at Eupper < 20 K, while 11 proto-BDs also show emission in the higher excitation lines at Eupper ∼21-49 K and ncrit ∼ 105 to 108 cm−3. In comparison with the brown dwarf formation models, the high excitation lines likely probe the warm (∼25-50 K) corino region at ∼10-50 au in the proto-BDs, while the low-excitation lines trace the cold (< 20 K) gas at ∼50-150 au. The column density for the cold component is an order of magnitude higher than the warm component. The CH3OH ortho-to-para ratios range between ∼0.3-2.3. The volume-averaged CH3OH column densities show a rise with decreasing bolometric luminosity among the proto-BDs, with the median column density higher by a factor of ∼3 compared to low-mass protostars. Emission in high-excitation (Eupper > 25 K) CH3OH lines together with the model predictions suggest that a warm corino is present in ∼78% of the proto-BDs in our sample. The remaining show evidence of only the cold component, possibly due to the absence of a strong, high-velocity jet that can stir up the warm gas around it.
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