Desorption Kinetics and Binding Energies of Small Hydrocarbons
| العنوان: | Desorption Kinetics and Binding Energies of Small Hydrocarbons |
|---|---|
| المؤلفون: | Aida Behmard, Mahesh Rajappan, Edith C. Fayolle, Pavlo Maksyutenko, Jennifer B. Bergner, Karin I. Öberg, Rafael Martín-Doménech, Dawn Graninger |
| بيانات النشر: | Zenodo, 2019. |
| سنة النشر: | 2019 |
| مصطلحات موضوعية: | Earth and Planetary Astrophysics (astro-ph.EP), chemistry.chemical_classification, Alkane, Physics, Astrochemistry, 010504 meteorology & atmospheric sciences, Thermal desorption spectroscopy, Binding energy, FOS: Physical sciences, Astronomy and Astrophysics, astrochemistry – methods: laboratory: molecular – protoplanetary disks, 01 natural sciences, Hydrocarbon, chemistry, Space and Planetary Science, Desorption, 0103 physical sciences, Physical chemistry, Alkene binding, Sublimation (phase transition), 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences |
| الوصف: | Small hydrocarbons are an important organic reservoir in protostellar and protoplanetary environments. Constraints on desorption temperatures and binding energies of such hydrocarbons are needed for accurate predictions of where these molecules exist in the ice vs. gas-phase during the different stages of star and planet formation. Through a series of temperature programmed desorption (TPD) experiments, we constrain the binding energies of 2 and 3-carbon hydrocarbons (C$_{2}$H$_{2}$ - acetylene, C$_{2}$H$_{4}$ - ethylene, C$_{2}$H$_{6}$ - ethane, C$_{3}$H$_{4}$ - propyne, C$_{3}$H$_{6}$ - propene, and C$_{3}$H$_{8}$ - propane) to 2200-4200 K in the case of pure amorphous ices, to 2400-4400 K on compact amorphous H$_{2}$O, and to 2800-4700 K on porous amorphous H$_{2}$O. The 3-carbon hydrocarbon binding energies are always larger than the 2-carbon hydrocarbon binding energies. Within the 2- and 3-carbon hydrocarbon families, the alkynes (i.e., least-saturated) hydrocarbons exhibit the largest binding energies, while the alkane and alkene binding energies are comparable. Binding energies are $\sim$5-20% higher on water ice substrates compared to pure ices, which is a small increase compared to what has been measured for other volatile molecules such as CO and N$_{2}$. Thus in the case of hydrocarbons, H$_{2}$O has a less pronounced effect on sublimation front locations (i.e., snowlines) in protoplanetary disks. 12 pages, 15 figures. Accepted for publication in The Astrophysical Journal |
| وصف الملف: | application/pdf |
| اللغة: | English |
| الوصول الحر: | https://explore.openaire.eu/search/publication?articleId=doi_dedup___::f2cdfe5a5699e2b3112e0b1071d9d2d3Test https://zenodo.org/record/2649397Test |
| حقوق: | OPEN |
| رقم الانضمام: | edsair.doi.dedup.....f2cdfe5a5699e2b3112e0b1071d9d2d3 |
| قاعدة البيانات: | OpenAIRE |
| الوصف غير متاح. |