Effect of Binding Energies on the Encounter Desorption
Artikel i vetenskaplig tidskrift, 2021

The abundance of interstellar ice constituents is usually expressed with respect to the water ice because, in denser regions, a significant portion of the interstellar grain surface would be covered by water ice. The binding energy (BE) or adsorption energy of the interstellar species regulates the chemical complexity of the interstellar grain mantle. Due to the high abundance of water ice, the BE of surface species with the water is usually provided and widely used in astrochemical modeling. However, the hydrogen molecules would cover some part of the grain mantle in the denser and colder part of the interstellar medium. Even at around similar to 10 K, few atoms and simple molecules with lower adsorption energies can migrate through the surface. The BE of the surface species with H-2 substrate would be very different from that of a water substrate. However, adequate information regarding these differences is lacking. Here, we employ the quantum chemical calculation to provide the BE of 95 interstellar species with H-2 substrate. These are representative of the BEs of species to a H-2 overlayer on a grain surface. On average, we notice that the BE with the H-2 monomer substrate is almost ten times lower than the BE of these species reported earlier with the H2O c-tetramer configuration. The encounter desorption of H and H-2 was introduced [with E-D (H, H-2) = 45 K and E-D (H-2, H-2) = 23 K] to have a realistic estimation of the abundances of the surface species in the colder and denser region. Our quantum chemical calculations yield higher adsorption energy of H-2 than that of H [E-D (H, H-2) = 23-25 K and E-D (H-2, H-2) = 67-79 K]. We further implement an astrochemical model to study the effect of encounter desorption with the present realistic estimation. The encounter desorption of the N atom [calculations yield E-D (N, H-2) = 83 K] is introduced to study the differences with its inclusion.

Monte Carlo (MC) algorithm

chemical model

ISM

astrochemistry

numerical

binding energy

star formation

Författare

Ankan Das

Indian Centre for Space Physics

Milan Sil

Indian Centre for Space Physics

Rana Ghosh

Indian Centre for Space Physics

Prasanta Gorai

Chalmers, Rymd-, geo- och miljövetenskap, Astronomi och plasmafysik, Extragalaktisk astrofysik

Soutan Adak

Ramakrishna Mission Residential College

Subhankar Samanta

Ramakrishna Mission Residential College

Sandip K. Chakrabarti

Indian Centre for Space Physics

FRONTIERS IN ASTRONOMY AND SPACE SCIENCES

2296-987X (ISSN)

Vol. 8 671622

Ämneskategorier

Oorganisk kemi

Annan kemi

Teoretisk kemi

DOI

10.3389/fspas.2021.671622

Mer information

Senast uppdaterat

2021-06-29