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N-bearing molecules (like N2H+ or NH3) are excellent tracers of high-density, low-temperature regions like dense cloud cores and could shed light into snowlines in protoplanetary disks and the chemical evolution of comets. However, uncertainties exist about the grain surface chemistry of these molecules -- which could play an important role in their formation and evolution. This study explores experimentally the behaviour of NH$_3$ on surfaces mimicking grains under interstellar conditions alongside other major interstellar ice components (ie. H$_2$O, CO, CO$_2$). We performed co-deposition experiments using the Ultra High Vacuum (UHV) setup VENUS (VErs des NoUvelles Syntheses) of NH$_3$ along with other adsorbates (here, H$_2$O, $^{13}$CO and CO$_2$) and performed Temperature Programmed Desorption (TPD) and Temperature Programmed-During Exposure Desorption (TP-DED) experiments. We obtained binding Energy (BE) distribution of NH$_3$ on Crystalline Ice(CI) and compact-Amorphous Solid Water (c-ASW) by analyses of the TPD profiles of NH3 on the substrates. We observe a significant delay in the desorption and a decrease in the desorption rate of NH$_3$ when H$_2$O is introduced into the co-deposited mixture of NH$_3$-$^{13}$Co or NH$_3$-CO$_2$, absent without H$_2$O. Secondly, H$_2$O traps nearly 5-9 per cent of the co-deposited NH3, released during water's amorphous-to-crystalline phase change. Thirdly, for CI, we obtained a BE distribution between 3780K-4080K, and c-ASW between 3780K-5280K -- using a pre-exponential factor A = 1.94$\times 10^{15}$/s. We conclude that NH$_3$ behaviour is significantly influenced by the presence of H$_2$O due to the formation of hydrogen bonds, in line with quantum calculations. This interaction preserves NH$_3$ on grain surfaces to higher temperatures making it available to the central protostar in protoplanetary disks. It also explains why NH$_3$ freeze out in pre-stellar cores is efficient.

Context. The nitrogen reservoir in planetary systems is a long standing problem. Part of the N-bearing molecules is probably incorporated into the ice bulk during the cold phases of the stellar evolution, and may be gradually released into the gas phase when the ice is heated, such as in active comets. The chemical nature of the N-reservoir should greatly influence how, when and in what form N returns to the gas phase, or is incorporated into the refractory material forming planetary bodies. Aims. We present the study the thermal desorption of two ammonium salts: ammonium formate and ammonium acetate from a gold surface and from a water ice substrate. Methods. Temperature-programmed desorption experiments and Fourier transform infrared reflection spectroscopy were conducted to investigate the desorption behavior of ammonium salts. Results. Ammonium salts are semi-volatile species releasing neutral species as major components upon desorption, that is ammonia and the corresponding organic acid (HCOOH and CH3COOH), at temperatures higher than the temperature of thermal desorption of water ice. Their desorption follows a first-order Wigner-Polanyi law. We find the first order kinetic parameters A = 7.7 $\pm$ 0.6 $\times$ 10$^{15}$ s$^{-1}$ and E$_{bind}$ = 68.9 $\pm$ 0.1 kJ~mol$^{-1}$ for ammonium formate and A = 3.0 $\pm$ 0.4 $\times$ 10$^{20}$ s$^{-1}$ and E$_{bind}$ = 83.0 $\pm$ 0.2 kJ~mol$^{-1}$ for ammonium acetate. The presence of a water ice substrate does not influence the desorption kinetics. Ammonia molecules locked in salts desorb as neutral molecules at temperatures much higher than previously expected that are usually attributed to refractory materials. Conclusions. Ammonia snow-line has a smaller radius than the water snow-line. As a result, the NH3/H2O ratio content in solar system bodies can be a hint as to where they formed and subsequently migrated., Comment: Accepted for publication in A&A, 10 pages, 7 figures

Two mooring lines equipped with near-bottom sediment traps were deployed in the axis of the Nazare submarine canyon at similar to 1600 and similar to 3300 m depth, respectively. We studied time-series of particle flux, composition (biogenic silica, carbonates, organic matter and lithogenic fractions), granulometry, mineralogy and Pb-210 concentration of particulate matter over five sediment trap deployments between October 2002 and December 2004. Current meters equipped with turbidimeters were also deployed at trap depths to monitor the water flow, temperature, salinity and suspended particle concentration. The composition of the collected particles was fairly constant year-round, dominated by the lithogenic fraction and with OC/N ratios in the range 11-21, suggesting an important terrigenous influence inside the canyon. The results show contrasting dynamic environments in the upper (1600 m depth) and middle (3300 m depth) canyon. High current speeds (spring tides up to 80 cm s(-1)) and high apparent mass fluxes of particulate matter (mean 65 g m(-2) d(-1); maximum 265 g m(-2) d(-1)) are permanent at the shallowest station. At the deepest site, fluxes were below 10 g m(-2) d(-1) most of the time and the annual flux was governed by events of sharp flux increase. Storms affecting the continental shelf during autumn and winter are a major driver of down-canyon dispersal of sediments to the middle canyon and beyond. Important nepheloid activity developed inside the canyon in response to storms with significant wave heights between 4 and 6 m, as testified by turbidimeters deployed in midwater and near the seabed at 1600 m water depth. On three occasions during the study period, significant wave heights of incident storms surpassed 7 m, leading to notable episodes of down-canyon transport that were clearly observed in the middle canyon. During one of these stormy periods (January 2003) a sediment gravity flow transporting unusual quantities of sand and coastal plant debri

Two mooring lines equipped with near-bottom sediment traps were deployed in the axis of the Nazare submarine canyon at similar to 1600 and similar to 3300 m depth, respectively. We studied time-series of particle flux, composition (biogenic silica, carbonates, organic matter and lithogenic fractions), granulometry, mineralogy and Pb-210 concentration of particulate matter over five sediment trap deployments between October 2002 and December 2004. Current meters equipped with turbidimeters were also deployed at trap depths to monitor the water flow, temperature, salinity and suspended particle concentration. The composition of the collected particles was fairly constant year-round, dominated by the lithogenic fraction and with OC/N ratios in the range 11-21, suggesting an important terrigenous influence inside the canyon. The results show contrasting dynamic environments in the upper (1600 m depth) and middle (3300 m depth) canyon. High current speeds (spring tides up to 80 cm s(-1)) and high apparent mass fluxes of particulate matter (mean 65 g m(-2) d(-1); maximum 265 g m(-2) d(-1)) are permanent at the shallowest station. At the deepest site, fluxes were below 10 g m(-2) d(-1) most of the time and the annual flux was governed by events of sharp flux increase. Storms affecting the continental shelf during autumn and winter are a major driver of down-canyon dispersal of sediments to the middle canyon and beyond. Important nepheloid activity developed inside the canyon in response to storms with significant wave heights between 4 and 6 m, as testified by turbidimeters deployed in midwater and near the seabed at 1600 m water depth. On three occasions during the study period, significant wave heights of incident storms surpassed 7 m, leading to notable episodes of down-canyon transport that were clearly observed in the middle canyon. During one of these stormy periods (January 2003) a sediment gravity flow transporting unusual quantities of sand and coastal plant debri