Influence of filter age on Fe, Mn and NH4+ removal in dual media rapid sand filters used for drinking water production

Rapid sand filtration is a common method for removal of iron (Fe), manganese (Mn) and ammonium (NH4+) from anoxic groundwaters used for drinking water production. In this study, we combine geochemical and microbiological data to assess how filter age influences Fe, Mn and NH4+ removal in dual media filters, consisting of anthracite overlying quartz sand, that have been in operation for between ∼2 months and ∼11 years. We show that the depth where dissolved Fe and Mn removal occurs is reflected in the filter medium coatings, with ferrihydrite forming in the anthracite in the top of the filters ( 1 m). Removal of NH4+ occurs through nitrification in both the anthracite and sand and is the key driver of oxygen loss. Removal of Fe is independent of filter age and is always efficient (> 97% removal). In contrast, for Mn, the removal efficiency varies with filter age, ranging from 9 to 28% at ∼2–3 months after filter replacement to 100% after 8 months. After 11 years, removal reduces to 60–80%. The lack of Mn removal in the youngest filters (at 2–3 months) is likely the result of a relatively low abundance of mineral coatings that adsorb Mn2+ and provide surfaces for the establishment of a microbial community. 16S rRNA gene amplicon sequencing shows that Gallionella, which are known Fe2+ oxidizers, are present after 2 months, yet Fe2+ removal is mostly chemical. Efficient NH4+ removal (> 90%) establishes within 3 months of operation but leakage occurs upon high NH4+loading (> 160 µM). Two-step nitrification by Nitrosomonas and Candidatus Nitrotoga is likely the most important NH4+ removal mechanism in younger filters during ripening (2 months), after which complete ammonia oxidation by Nitrospira and canonical two-step nitrification occur simultaneously in older filters. Our results highlight the strong effect of filter age on especially Mn2+but also NH4+ removal. We show that ageing of filter medium leads to the development of thick coatings, which we hypothesize leads to preferential flow, and breakthrough of Mn2+. Use of age-specific flow rates may increase the contact time with the filter medium in older filters and improve Mn2+ and NH4+ removal

The role of water in planet formation

Planet formation takes place in gaseous disks around young stars. Exactly how small dust particles in such protoplanetary disks turn into rocky planets and the cores of gas giants is not known. In particular, the formation of planetesimals (kilometer-sized objects akin to asteroids, considered to be an important intermediate step in the planet formation process) is still highly elusive. A promising mechanism for planetesimal formation is the streaming instability. Under certain conditions, dense filaments of pebbles (solid particles that are aerodynamically partly decoupled from the gas disk) can emerge as a result of this instability. Clumps of pebbles may subsequently collapse under their own gravity to form planetesimals. In this thesis, the growth and dynamics of dust particles and the viability of streaming instability being triggered close to the water snowline — the distance from the star beyond which water freezes out — are explored with numerical models. Additionally, a reported ALMA observation of the water snowline around an outbursting star is discussed in light of these models. Finally, a model that connects the two main stages of planet formation, from dust to planetesimals and from planetesimals to planets, is developed. This model is applied to the formation of the TRAPPIST-1 system; a compact system with seven Earth-sized planets that are expected to have moderate water fractions of a few mass percent. It is shown that local planetesimal formation at the water snowline followed by inward migration of protoplanets naturally leads to such planets

Dark matter subhalos and unidentified sources in the Fermi 3FGL source catalog

If dark matter consists of weakly interacting massive particles (WIMPs), dark matter subhalos in the Milky Way could be detectable as gamma-ray point sources due to WIMP annihilation. In this work, we perform an updated study of the detectability of dark matter subhalos as gamma-ray sources with the Fermi Large Area Telescope (Fermi LAT). We use the results of the Via Lactea II simulation, scaled to the Planck 2015 cosmological parameters, to predict the local dark matter subhalo distribution. Under optimistic assumptions for the WIMP parameters—a 40 GeV particle annihilating to bb with a thermal cross-section, as required to explain the Galactic center GeV excess—we predict that at most ~ 10 subhalos might be present in the third Fermi LAT source catalog (3FGL). This is a smaller number than has been predicted by prior studies, and we discuss the origin of this difference. We also compare our predictions for the detectability of subhalos with the number of subhalo candidate sources in 3FGL, and derive upper limits on the WIMP annihilation cross-section as a function of the particle mass. If a dark matter interpretation could be excluded for all 3FGL sources, our constraints would be competitive with those found by indirect searches using other targets, such as known Milky Way satellite galaxies