Formation of hydrogen peroxide and water from the reaction of cold hydrogen atoms with solid oxygen at 10K

Abstract

The reactions of cold H atoms with solid O 2 molecules were investigated at 10 K. The formation of H 2 O 2 and H 2 O has been confirmed by in-situ infrared spectroscopy. We found that the reaction proceeds very efficiently and obtained the effective reaction rates. This is the first clear experimental evidence of the formation of water molecules under conditions mimicking those found in cold interstellar molecular clouds. Based on the experimental results, we discuss the reaction mechanism and astrophysical implications.

Solid state chemistry of nitrogen oxides – Part II: surface consumption of NO2

“…Water formation has been extensively studied in the solid phase over the past decade. [47][48][49][51][52][53][54][55][56] Fig. 1 and 2 show that NH 2 OH and H 2 O are the final products of the hydrogenation of NO 2 .…”

Water deuterium fractionation in the high-mass star-forming region G34.26+0.15 based on Herschel/HIFI data

“…demonstrated by Miyauchi et al (2008), Ioppolo et al (2008) and Oba et al (2009), or by hydrogenation of ozone:…”

Surface formation routes of interstellar molecules: hydrogenation reactions in simple ices

“…This approach makes it possible to derive fundamental and molecule specific parameters, like reaction rates and diffusion barriers, which can then be included in astrochemical models to simulate the ice evolution under much longer timescales (10 5 years) than accessible in the laboratory (\1 day). The work presented in the next section follows a bottom-up approach and summarizes a representative sample of relevant experiments (e.g., Watanabe and Kouchi 2002;Watanabe et al 2004Watanabe et al , 2006Fuchs et al 2009;Miyauchi et al 2008;Ioppolo et al 2008Ioppolo et al , 2010Ioppolo et al , 2011aMatar et al 2008;Oba et al 2009Oba et al , 2010Cuppen et al 2010;Mokrane et al 2009;Romanzin et al 2011;Ö berg et al 2009). These experiments prove that species like H 2 CO, CH 3 OH and H 2 O can be formed at low temperatures by simple hydrogenation (i.e., without the need for thermal, UV or cosmic ray processing) and provide the basic molecular data to simulate their formation on astronomical timescales (e.g., Cuppen et al 2009), even though the ice as a whole is not representative for a realistic astronomical ice.…”

“…All three hydrogenation channels have been investigated qualitatively by Dulieu et al (2010) in the submonolayer regime using TPD as their main analysis technique, confirming the formation of water ice. The hydrogenation of solid O 2 is the most extensively studied channel (e.g., Miyauchi et al 2008;Ioppolo et al 2008;Matar et al 2008). Ioppolo et al (2008) investigated this reaction channel for a large range of astronomically relevant temperatures (12-28 K).…”