Enhanced Deuterium Fractionation in Dense Interstellar Cores Resulting from Multiply Deuterated H3+

By H. Roberts, E. Herbst, T. Millar. 2003

221 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/118c0e2d66be89f29f7ab002cc57f1641b67b6a5

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. P. Caselli
2. E. Herbst
3. Cecilia Ceccarelli
4. E. Bergin
5. M. Tafalla
6. E. Dishoeck
7. H. Roberts
8. R. Garrod

In Atomic and Molecular Physics, and Optics

1. E. Bergin
2. M. Tafalla
3. P. Caselli
4. Cecilia Ceccarelli
5. E. Dishoeck
6. A. Tielens
7. E. Herbst
8. G. P. D. Forêts

In Spectroscopy

1. Cecilia Ceccarelli
2. P. Caselli
3. E. Herbst
4. E. Bergin
5. E. Dishoeck
6. M. Tafalla
7. J. Jørgensen
8. H. Roberts

Citations in the corpus

• Organic molecules in protoplanetary disks around T Tauri and Herbig Ae stars (2004, background): “…(Tielens 1983), although not for DCO+/HCO+. Recent chemical models succeed in explaining the high fractionation observed here and in dark cloud cores (Rodgers & Millar 1996; Roberts & Millar 2000, Tiné et al. 2000), but only if significant freeze-out is included (Roberts et al. 2002, 2003).”
• The chemistry of multiply deuterated species in cold, dense interstellar cores (2004, methodology): “In any case, at late times, the loss of deuterium from the gas-phase is much less catastrophic than in Roberts et al. (2003) because dissociative recombination of molecular ions on the grain surfaces also produces significant amounts of H, D, H2, HD and D2 which quickly evaporate.”
• Cold Dark Clouds: The Initial Conditions for Star Formation (2007, methodology): “…do not stop with H2D +, rather they continue towards the formation of both D2H + and D+3 , via a similar reaction sequence (Phillips & Vastel 2003; Roberts et al. 2003; Walmsley et al. 2004): H2D + + HD ↔ D2H + + H2 + 180K, (3) H2D + + HD ↔ D+3 + H2 + 230K. (4) (2) The freeze-out of CO, which is…”
• Chemical modeling of L183 (= L134N) : an estimate of the ortho/para H2 ratio (2008, background): “…HD forms H2D+ and this primary fractionation is then followed by the subsequent fractionations and produces D2H+ and D+3 (Phillips & Vastel 2003, Roberts et al. 2003) : H+3 + HD ←→ H2D + + H2 + 232 K (1) H2D + + HD ←→ D2H+ + H2 + 187 K (2) D2H+ + HD ←→ D+3 + H2 + 234 K. (3) The backward…”
• First detection of triply-deuterated methanol (2003, background): “Such a high atomic fractionation ratio in the gas phase is predicted by the recent gas-phase model of Roberts et al. (2003), which involves not only H2D + but also D2H + and D+3 as precursors for deuterium fractionation, when the density of gas is very high and heavy species such as CO are strongly…”
• Our astrochemical heritage (2012, background): “This deuteration “jump” allows multiply deuterated forms of H+3 to thrive (Vastel et al. 2004; Parise et al. 2011) and their dissociative recombinations with electrons liberate D atoms, locally increasing the D/H ratio to values larger than 0.1 (Roberts et al. 2003).”
• Testing grain surface chemistry : a survey of deuterated formaldehyde and methanol in low-mass Class 0 protostars (2006, background): “Furthermore, th bulk of the formaldehyde would be formed under undepleted conditions and hence the D2CO and HDCO fractionation is difficult to understand (Roberts et al. 2003).”
• Complete depletion in prestellar cores (2004, result): “Our results can be compared with those of Roberts et al. (2003) who carried out a time dependent calculation of the chemistry in a prestellar core with density 3 106 cm−3 including freeze–out.”
• Molecular inventories and chemical evolution of low-mass protostellar envelopes (2003, background): “Models by Roberts & Millar (2000a) and Roberts et al. (2003) show that a high degree of depletion may be required in order to produce formation of the doubly and triply deuterated species observed in protostellar environments (Ceccarelli et al. 1998; Lis et al. 2002; Parise et al. 2002; van der Tak…”
• The importance of the ortho:para H2 ratio for the deuteration of molecules during pre-protostellar collapse (2006, background): “The related reaction networks have been considered in detail by several authors (Roberts et al. 2003, 2004; Roueff et al. 2005).”