Abstract
After its successful campaign of measurements beyond the Polar Arctic Circle, the PolarquEEEst experiment measured the cosmic charged particle rate at sea level in a latitude interval ...between 35
$$^{\circ }$$
∘
N and 82
$$^{\circ }$$
∘
N. In this paper, these measurements are described and the corresponding results are discussed.
In this paper, we summarize the present state-of-the-art on the proof-of-principle experiment of frequency-dependent squeezing implemented through EPR entanglement for Virgo gravitational-wave ...detector and we introduce Virgo subsystem proposal for frequency-dependent squeezing, obtained with a compact apparatus and without the costs required by the infrastructure for the filter cavity.
We investigated the deposition of (HO)2-PO-S-(CH2)15-COOH on TiO2. The phosphonate group has been chosen to serve as the anchoring moiety while the carboxylic group can be exploited for further ...coupling with antibacterial peptides. Native oxide-covered polished Ti samples were used as substrates for the molecular deposition. Previous to deposition, the substrates were plasma-cleaned in order to enrich their surfaces of hydroxyl groups, suitable for phosphonate coupling. The combined analysis of atomic force microscopy, X-ray photoemission spectroscopy and differential spectroscopic ellipsometry measurements indicates the formation of a submonolayer film made of irregular islands, one molecule thick.
The surface chemical composition of Nb samples prepared by following procedures commonly employed in the preparation of RF cavities has been studied by XPS and ARXPS. In order to understand the ...process occurring at surface, the thermal evolution of the surface has been studied in the 30°C÷1000°C range of temperature both in the heating and cooling phases. During the heating phase, an irreversible transition has been observed near
T≅200÷300°C; it is characterized by a progressive reduction of Nb oxides from Nb
2O
5 to NbO
2 and finally to NbO. The O signal disappears near
T≅1000°C and it reappears below 900°C, during the cooling phase. This can be interpreted as due to O migration in the Nb matrix, raising
T, and to O diffusion towards the surface as the temperature decreases. Work function measurements show that the values of
Φ are strongly correlated with the chemical composition of the surface.
The Forbush decrease following the large X2 solar flare on mid-February 2011 has been observed by the muon telescopes of the EEE Project, which are located in several Italian sites and at CERN. Data ...from two different telescopes of the EEE network have been analyzed and compared to those measured by neutron monitor stations. The variation of the muon counting rate during the Forbush decrease was also extracted for different intervals of the azimuthal angle of the incoming muons.
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