Deuterated Methanol in the Orion Compact Ridge

Charnley, S. B.; Tielens, A. G. G. M.; Rodgers, S. D.

doi:10.1086/310697

Cited by 264 publications

(329 citation statements)

References 24 publications

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“…Atom addition reactions on dust, primarily starting from condensed CO, can lead to many organic compounds, such as formaldehyde, methanol, formic acid, acetaldehyde, isocyanic acid and formamide, molecules which are also identified in comets (e.g., Herbst and van Dishoeck 2009). High atomic D/H ratios in the condensing gas consequently leads to very high D/H ratios and the formation of many multiply-deuterated isotopologues for surface-formed molecules (Charnley et al 1997); these latter species include D 2 O, D 2 CO, CHD 2 OH, CD 3 OH, NHD 2 , ND 3 and D 2 S (Parise et al 2006;Ceccarelli et al 2014). These characteristics are observed in the interstellar medium and Table 4 summarizes the range of D/H ratios found in cold dark clouds and in cores forming both low-mass and massive protostars.…”

Section: Interstellar Isotopic Fractionationmentioning

confidence: 99%

“…These characteristics are observed in the interstellar medium and Table 4 summarizes the range of D/H ratios found in cold dark clouds and in cores forming both low-mass and massive protostars. In the latter regions the highest D/H ratios are due to highly-fractionated ices being evaporated from warm dust grains (e.g., Charnley et al 1997).…”

Section: Interstellar Isotopic Fractionationmentioning

confidence: 99%

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Cometary Isotopic Measurements

et al. 2015

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Section: Interstellar Isotopic Fractionationmentioning

confidence: 99%

Section: Interstellar Isotopic Fractionationmentioning

confidence: 99%

Cometary Isotopic Measurements

et al. 2015

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“…But observational evidences suggest that CH3OD is relatively less abundant in comparison to CH2DOH and fractionation ratio of CH3OD/CH3OH and CH2DOH/CH3OH would be 0.02(±0.01) and 0.3(±0.2) respectively in IRAS 16293-2422. Charnley , Tielens & Rodgers (1997) and Osamura, Roberts & Herbst (2004) discussed the possible interconversion between pairs of deuterated forms of methanol, its ion, and its proportionated ion in star-forming regions. They also suggested that CH3OD is comparatively less abundant than CH2DOH.…”

Section: Composition Of Grain Mantles With Deuterated Speciesmentioning

confidence: 99%

Deuterium enrichment of the interstellar grain mantle

Das¹,

Sahu²,

Majumdar³

et al. 2015

Mon. Not. R. Astron. Soc.

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We carry out Monte-Carlo simulation to study deuterium enrichments of interstellar grain mantles under various physical conditions. Based on the physical properties, various types of clouds are considered. We find that in diffuse cloud regions, very strong radiation fields persists and hardly a few layers of surface species are formed. In translucent cloud regions with a moderate radiation field, significant number of layers would be produced and surface coverage is mainly dominated by photo-dissociation products such as, C, CH 3 , CH 2 D, OH and OD. In the intermediate dense cloud regions (having number density of total hydrogen nuclei in all forms ∼ 2 × 10 4 cm −3 ), water and methanol along with their deuterated derivatives are efficiently formed. For much higher density regions (∼ 10 6 cm −3 ), water and methanol productions are suppressed but surface coverages of CO, CO 2 , O 2 , O 3 are dramatically increased. We find a very high degree of fractionation of water and methanol. Observational results support a high fractionation of methanol but surprisingly water fractionation is found to be low. This is in contradiction with our model results indicating alternative routes for de-fractionation of water. Effects of various types of energy barriers are also studied. Moreover, we allow grain mantles to interact with various charged particles (such as H + , Fe + , S + and C + ) to study the stopping power and projected range of these charged particles on various target ices.

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“…These molecules are known to exist abundantly in hot cores in high-mass star forming regions. Since the gas-phase chemical reactions cannot produce them efficiently, they are thought to be formed by grain surface reactions (e.g., Charnley et al 1997;Watanabe & Kouchi 2002;Garrod & Herbst 2006;Herbst & van Dishoeck 2009). The produced molecules stay on grain mantles in the cold phase, and they are librated into the gas phase after the birth of high-mass stars.…”

Section: Introductionmentioning

confidence: 99%

Observations of Complex Molecules in Low-Mass Protostars

Sakai

Yamamoto

2011

Proc. IAU

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Abstract. Low-mass star forming regions are rich inventories of complex organic molecules. Furthermore, they show significant chemical diversity even among sources in a similar physical evolutionary stage (i.e. Class 0 sources). One distinct case is the hot corino chemistry characterized by rich existence of saturated complex organic molecules such as HCOOCH3 and C2 H5 CN, whereas the other is the warm carbon-chain chemistry (WCCC) characterized by extraordinary richness of unsaturated complex organic molecules such as carbon-chain molecules. We here summarize these observational achievements during the last decade, and present a unified picture of carbon chemistry in low-mass protostellar cores. The chemical diversity most likely originates from the source-to-source difference in chemical compositions of grain mantles. In particular, the gas-phase abundance of CH 4 evaporated from grain mantles is thought to be a key factor for appearance of WCCC. The origin of the diversity and its evolution to protopranetary disks are discussed.

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Deuterated Methanol in the Orion Compact Ridge

Cited by 264 publications

References 24 publications

Cometary Isotopic Measurements

Cometary Isotopic Measurements

Deuterium enrichment of the interstellar grain mantle

Observations of Complex Molecules in Low-Mass Protostars

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