A laboratory survey of the thermal desorption of astrophysically relevant molecules

By M. Collings, Mark R. Anderson, Rui Chen, John W. Dever, S. Viti, David A. Williams, M. McCoustra. 2004

454 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/c75038bf999ca7057aa0fccec7ddc5f5fee87b1c

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. R. Garrod
2. E. Dishoeck
3. K. Oberg
4. E. Bergin
5. Simon Bruderer
6. E. Herbst
7. V. Wakelam
8. P. Caselli

In Atmospheric Science

1. R. Garrod
2. E. Dishoeck
3. E. Herbst
4. V. Wakelam
5. E. Bergin
6. K. Oberg
7. H. Cuppen
8. M. Ruaud

In Spectroscopy

1. R. Garrod
2. E. Dishoeck
3. E. Herbst
4. V. Wakelam
5. K. Oberg
6. E. Bergin
7. E. V. van Dishoeck
8. C. Dullemond

Citations in the corpus

• Reaction Networks for Interstellar Chemical Modelling: Improvements and Challenges (2010, background): “…for thermal evaporation, which is normally unimportant in the cold interstellar medium but increases in importance at higher temperatures (Collings et al. 2004), it is dN(A)/dt = −kevap,AN(A), (31) where the rate coefficient is the same as that for hopping except that the barrier is…”
• Complex organic molecules in protoplanetary disks (2013, background): “(1) Collings et al. (2004); (2) Garrod & Herbst (2006); (3) Cuppen & Herbst (2007). from both UV and X-ray photons; however, cosmic rays are able to penetrate the entire disk.”
• The chemical history of molecules in circumstellar disks - I. Ices (2009, background): “Recent laboratory experiments suggest that CO desorbs from a CO-H2O ice in four steps (Collings et al. 2004).”
• Non-thermal desorption from interstellar dust grains via exothermic surface reactions (2007, methodology): “For example, the new CR-induced desorption rate for methanol is negligible, using the measured binding energy of 5530 K (Collings et al. 2004).”
• Complex Chemistry in Star-forming Regions: An Expanded Gas-Grain Warm-up Chemical Model (2008, methodology): “As in GH06, we interpolate experimental binding energy values for certain key species (Collings et al. 2004) by simple – 8 – addition or subtraction, to produce values for all other species in our set.”
• Direct mapping of the temperature and velocity gradients in discs Imaging the vertical CO snow line around IM Lupi (2017, background): “…17 K; Zhang et al. 2017: 27 K) and the Herbig Ae star HD 163296 (Qi et al. 2011: 19 K, Mathews et al. 2013: 19 K; Qi et al. 2015: 25 K), where freeze-out temperatures higher than 25 K would suggest ice mixtures where the binding energy is higher (Collings et al. 2003, 2004; Noble et al. 2012).”
• Formation of methyl formate and other organic species in the warm-up phase of hot molecular cores (2006, methodology): “We use these values and add to them data provided by Dr. M. P. Collings (private communication), which correspond to the TPD results obtained by Collings et al. (2004).”
• Ice structures, patterns, and processes: A view across the icefields (2012, background): “An experimental survey shows that the desorption of a variety of different volatile molecules under these interstellar conditions can be broadly classified by the nature of their interaction with the water molecules that make up the ASW host (Collings et al., 2004).”
• Sulphur-bearing species in the coma of comet 67P/Churyumov–Gerasimenko (2016, background): “The sublimation temperature of pure H2S ice in ultrahigh vacuum is 80 K (Collings et al. 2004).”
• Grain Surface Models and Data for Astrochemistry (2017, background): “Collings et al. (2004) showed, for instance, that a fraction of molecules like CO and CO2 can become trapped in an ice mantle which consists predominantly of water ice.”
• Binding energies: New values and impact on the efficiency of chemical desorption (2017, methodology): “…et al. 2016) 2400 (Hama & Watanabe 2013) 2860 (Sandford & Allamandola 1990) 2575 (Collings et al. 2004) OCS 2100 2400 2888 2430 (Ward et al. 2012) 2888 (Collings et al. 2004) N 1200 900 720 800 720 (Minissale et al. 2016) NH 2800 2400 2600 2378 3000 2800 NH2 2800 2500 3200 3956 4500 4100 NH3 5600…”
• Formation rates of complex organics in UV irradiated CH3OH-rich ices I: Experiments (2009, methodology): “The values agree with those published by Garrod & Herbst (2006), based on experiments on water rich ice mixtures by Collings et al. (2004), within 20%, except for HCOOCH3 where the discrepancy is larger.”
• THE EFFECTS OF SNOWLINES ON C/O IN PLANETARY ATMOSPHERES (2011, background): “For all other molecules, we calculate the density-dependent sublimation temperatures following the prescription of Hollenbach et al. (2009) using binding energies of H2O, CO2 and CO of 5800 K, 2000 K and 850 K (Collings et al. 2004; Fraser et al. 2001; Aikawa et al. 1996).”
• The UMIST database for astrochemistry 2012 (2012, methodology): “…& Tielens (2002), Chastaing et al. (2000), Chastaing et al. (1998), Chastaing et al. (1999), Chastaing et al. (1999), Cohen & Westberg (1991), Collings et al. (2004), Cordiner & Millar (2009), Dalgarno et al. (1990), Danielsson et al. (2008), Daugey et al. (2005), Daugey et al. (2008),…”
• Desorption rates and sticking coefficients for CO and N2 interstellar ices (2006, background): “The desorption behavior will thus also be quite similar for CO and N2 in mixed or layered ices with H2O as is observed in the TPD experiments by Collings et al. (2004), where both species desorb in multiple steps.”
• Chemistry in Disks. IV. Benchmarking gas-grain chemical models with surface reactions (2010, background): “We do not distinguish between various thermal evaporation scenarios for different molecules, e.g. via “volcanic” or multilayer desorption (Collings et al., 2004).”
• THE SPITZER ICE LEGACY: ICE EVOLUTION FROM CORES TO PROTOSTARS (2011, methodology): “The CO:H2O contents toward low and high mass objects are comparable, consistent with experiments that show that 5–10% of CO can be trapped in H2O ice up to the H2O evaporation temperature (Sandford & Allamandola 1990; Collings et al. 2004; Fayolle et al. 2011).”
• Testing grain-surface chemistry in massive hot-core regions (2007, background): “Laboratory experiments indicate that it only evaporates at very high temperatures (∼100 K) similar to H2O (Collings et al. 2004).”