426 research outputs found
Mantle wedge temperatures and their potential relation to volcanic arc location
The mechanisms underpinning the formation of a focused volcanic arc above subduction zones are debated. Suggestions include controls by: (i) where the subducting plate releases water, lowering the solidus in the overlying mantle wedge; (ii) the location where the mantle wedge melts to the highest degree; and (iii) a limit on melt formation and migration imposed by the cool shallow corner of the wedge. Here, we evaluate these three proposed mechanisms using a set of kinematically-driven 2D thermo-mechanical mantle-wedge models in which subduction velocity, slab dip and age, overriding-plate thickness and the depth of decoupling between the two plates are systematically varied. All mechanisms predict, on the basis of model geometry, that the arc-trench distance, D, decreases strongly with increasing dip, consistent with the negative D-dip correlations found in global subduction data. Model trends of sub-arc slab depth, H, with dip are positive if H is wedge-temperature controlled and overriding-plate thickness does not exceed the decoupling depth by more than 50 km, and negative if H is slab-temperature controlled. Observed global H-dip trends are overall positive. With increasing overriding plate thickness, the position of maximum melting shifts to smaller H and D, while the position of the trenchward limit of the melt zone, controlled by the wedge's cold corner, shifts to larger H and D, similar to the trend in the data for oceanic subduction zones. Thus, the limit imposed by the wedge corner on melting and melt migration seems to exert the first-order control on arc position
Reduction of myocardial infarction by postischemic administration of the calpain inhibitor A-705253 in comparison to the Na(+)/H(+) exchange inhibitor Cariporide (R) in isolated perfused rabbit hearts
The calpain inhibitor A-705253 and the Na(+)/H(+) exchange inhibitor Cariporide (R) were studied in isolated perfused rabbit hearts subjected to 60 min occlusion of the ramus interventricularis of the left coronary artery (below the origin of the first diagonal branch), followed by 120 min of reperfusion. The inhibitors were added to the perfusion fluid solely or in combination at the beginning of reperfusion. Hemodynamic monitoring and biochemical analysis of perfusion fluid from the coronary outflow were performed. Myocardial infarct size and area at risk (transiently not perfused myocardium) were determined from left ventricular slices after a special staining procedure with Evans blue and 2,3,5-triphenyltetrazolium chloride. The infarcted area (dead myocardium) was 72.7 +/- 4.0% of the area at risk in untreated controls, but was significantly smaller in the presence of the inhibitors. The largest effect was observed with 10(-6) M A-705253, which reduced the infarcted area to 49.2 +/- 4.1% of the area at risk, corresponding to a reduction of 33.6%. Cariporide (R) at 10(-6) M reduced the infarct size to the same extent. The combination of both inhibitors, however, did not further improve cardioprotection. No significant difference was observed between the experimental groups in coronary perfusion, left ventricular pressure, heart rate, or in the release of lactate dehydrogenase and creatine kinase from heart muscle
High-contrast imaging constraints on gas giant planet formation - The Herbig Ae/Be star opportunity
Planet formation studies are often focused on solar-type stars, implicitly
considering our Sun as reference point. This approach overlooks, however, that
Herbig Ae/Be stars are in some sense much better targets to study planet
formation processes empirically, with their disks generally being larger,
brighter and simply easier to observe across a large wavelength range. In
addition, massive gas giant planets have been found on wide orbits around early
type stars, triggering the question if these objects did indeed form there and,
if so, by what process. In the following I briefly review what we currently
know about the occurrence rate of planets around intermediate mass stars,
before discussing recent results from Herbig Ae/Be stars in the context of
planet formation. The main emphasis is put on spatially resolved polarized
light images of potentially planet forming disks and how these images - in
combination with other data - can be used to empirically constrain (parts of)
the planet formation process. Of particular interest are two objects, HD100546
and HD169142, where, in addition to intriguing morphological structures in the
disks, direct observational evidence for (very) young planets has been
reported. I conclude with an outlook, what further progress we can expect in
the very near future with the next generation of high-contrast imagers at 8-m
class telescopes and their synergies with ALMA.Comment: Accepted by Astrophysics and Space Science as invited short review in
special issue about Herbig Ae/Be stars; 12 pages incl. 5 figures, 2 tables
and reference
Bulk micromegas detectors for large TPC applications
A large volume TPC will be used in the near future in a variety of experiments including T2K. The bulk Micromegas detector for this TPC is built using a novel production technique particularly suited for compact and robust low mass detectors. The capability to pave a large surface with a simple mounting solution and small dead space between modules is of particular interest for these applications. We have built several large bulk Micromegas detectors (27 x 26 cm2) and we have tested them in the former HARP field cage setup with a magnetic field. Cosmic ray data have been acquired in a variety of experimental conditions. Good detector performances and space point resolution have been achieved
Analysis of the modes of energy consumption of the complex of an incoherent scattering of the institute of ionosphere of national academy of sciences and the ministry of education and science of Ukraine
ĐŁ ĐŽĐ°ĐœŃĐč ŃŃĐ°ŃŃŃ ĐżŃДЎŃŃĐ°ĐČĐ»Đ”ĐœŃ ŃДзŃĐ»ŃŃĐ°ŃĐž Đ°ĐœĐ°Đ»ŃĐ·Ń ŃĐ”Đ¶ĐžĐŒŃĐČ Đ”ĐœĐ”ŃĐłĐŸŃĐżĐŸĐ¶ĐžĐČĐ°ĐœĐœŃ ĐșĐŸĐŒĐżĐ»Đ”ĐșŃŃ ĐœĐ”ĐșĐŸĐłĐ”ŃĐ”ĐœŃĐœĐŸĐłĐŸ ŃĐŸĐ·ŃŃŃĐœĐœŃ ĐĐœŃŃĐžŃŃŃŃ ŃĐŸĐœĐŸŃŃĐ”ŃĐž ĐĐĐ Ń ĐĐĐ ĐŁĐșŃĐ°ŃĐœĐž Đ· ĐŒĐ”ŃĐŸŃ ĐČĐžŃŃŃĐ”ĐœĐœŃ ĐżŃĐŸĐ±Đ»Đ”ĐŒĐž ĐżŃĐŽĐČĐžŃĐ”ĐœĐœŃ Đ”ĐœĐ”ŃĐłĐŸĐ”ŃĐ”ĐșŃĐžĐČĐœĐŸŃŃŃ ĐœĐ°ŃĐșĐŸĐČĐŸ-ĐŽĐŸŃĐ»ŃĐŽĐœĐŸĐłĐŸ ĐșĐŸĐŒĐżĐ»Đ”ĐșŃŃ ŃĐ° ŃŃĐČĐŸŃĐ”ĐœĐœŃ Đ”ĐœĐ”ŃĐłĐŸĐ”ŃĐ”ĐșŃĐžĐČĐœĐŸŃ ŃĐžŃŃĐ”ĐŒĐž ДлДĐșŃŃĐŸĐżĐŸŃŃĐ°ŃĐ°ĐœĐœŃ, ŃĐșĐ° забДзпДŃĐžŃŃ ŃŃŃĐčĐșŃ ŃĐŸĐ±ĐŸŃŃ ĐœĐ°ŃĐșĐŸĐČĐŸĐłĐŸ ĐŸĐ±Đ»Đ°ĐŽĐœĐ°ĐœĐœŃ ĐŽĐ»Ń ĐČĐžĐșĐŸĐœĐ°ĐœĐœŃ ĐŽĐŸŃĐ»ŃĐŽĐœĐžŃŃĐșĐžŃ
ĐżŃĐŸĐłŃĐ°ĐŒ ĐĐĐ ĐŁĐșŃĐ°ŃĐœĐž. ĐпОŃĐ°ĐœĐ° ŃĐžŃŃĐ”ĐŒĐ° ДлДĐșŃŃĐŸĐ¶ĐžĐČĐ»Đ”ĐœĐœŃ ĐșĐŸĐŒĐżĐ»Đ”ĐșŃŃ ŃĐ° ŃĐ”Đ¶ĐžĐŒĐž Đ”ĐœĐ”ŃĐłĐŸŃĐżĐŸĐ¶ĐžĐČĐ°ĐœĐœŃ ĐșĐŸĐŒĐżĐ»Đ”ĐșŃŃ. ĐпОŃĐ°ĐœĐŸ ĐżŃĐžŃŃŃĐŸŃ ŃĐ°ĐŽĐ°ŃĐœĐŸŃ ŃĐžŃŃĐ”ĐŒĐž, Đ° ŃĐ°ĐșĐŸĐ¶ ĐœĐ°ĐčбŃĐ»ŃŃ ĐżĐŸŃŃĐ¶ĐœŃ ŃĐżĐŸĐ¶ĐžĐČĐ°ŃŃ Đ”Đ»Đ”ĐșŃŃĐŸĐ”ĐœĐ”ŃĐłŃŃ, ŃĐșŃ ŃĐżĐŸĐ¶ĐžĐČĐ°ŃŃŃ Đ”Đ»Đ”ĐșŃŃĐŸĐ”ĐœĐ”ŃĐłŃŃ ĐœĐ° Đ”ĐșŃпДŃĐžĐŒĐ”ĐœŃĐ°Đ»ŃĐœŃ Ń ĐłĐŸŃĐżĐŸĐŽĐ°ŃŃŃĐșŃ ĐżĐŸŃŃДбО. ĐŃĐŸĐ°ĐœĐ°Đ»ŃĐ·ĐŸĐČĐ°ĐœĐŸ Đ”ĐœĐ”ŃĐłĐŸŃĐżĐŸĐ¶ĐžĐČĐ°ĐœĐœŃ ĐșĐŸĐŒĐżĐ»Đ”ĐșŃŃ ĐœĐ”ĐșĐŸĐłĐ”ŃĐ”ĐœŃĐœĐŸĐłĐŸ ŃĐŸĐ·ŃŃŃĐœĐœŃ Đ·Đ° 2013 Ń. ĐŃŃĐžĐŒĐ°ĐœĐŸ Ń ĐżŃДЎŃŃĐ°ĐČĐ»Đ”ĐœĐŸ ĐłŃĐ°ŃŃĐșĐž ŃĐ”ŃĐ”ĐŽĐœŃĐŸŃ ŃĐżĐŸĐ¶ĐžĐČĐ°ĐœĐŸŃ ĐżĐŸŃŃĐ¶ĐœĐŸŃŃŃ (ŃĐ”ŃĐ”ĐŽĐœŃĐŸĐŽĐŸĐ±ĐŸĐČĐžĐč ĐżĐŸĐșĐ°Đ·ĐœĐžĐș) Ń ŃĐ”ŃĐ”ĐŽĐœŃĐŸŃ ŃĐżĐŸĐ¶ĐžĐČĐ°ĐœĐŸŃ ĐżĐŸŃŃĐ¶ĐœĐŸŃŃŃ ĐČ ŃĐ”Đ¶ĐžĐŒŃ ĐČĐžĐŒŃŃŃĐČĐ°ĐœŃ. ĐпОŃĐ°ĐœĐ° ĐŽĐŸŃŃĐ»ŃĐœŃŃŃŃ ĐżŃĐŸĐČĐ”ĐŽĐ”ĐœĐœŃ ŃĐŸĐ±ŃŃ Đ· ĐŸĐżŃĐžĐŒŃĐ·Đ°ŃŃŃ Đ”ĐœĐ”ŃĐłĐŸĐżĐŸŃŃĐ°ŃĐ°ĐœĐœŃ ĐœĐ°ŃĐșĐŸĐČĐŸ-ĐŽĐŸŃĐ»ŃĐŽĐœĐŸĐłĐŸ ĐșĐŸĐŒĐżĐ»Đ”ĐșŃŃ ĐĐœŃŃĐžŃŃŃŃ ŃĐŸĐœĐŸŃŃĐ”ŃĐž. ĐĐ°ĐżŃĐŸĐżĐŸĐœĐŸĐČĐ°ĐœĐŸ ĐŒĐŸĐ¶Đ»ĐžĐČŃ Đ·Đ°Ń
ĐŸĐŽĐž ĐŽĐ»Ń Đ·ĐœĐžĐ¶Đ”ĐœĐœŃ Đ”ĐșĐŸĐœĐŸĐŒŃŃĐœĐŸŃ ĐČĐ°ŃŃĐŸŃŃŃ ĐżŃĐŸĐČĐ”ĐŽĐ”ĐœĐœŃ Đ”ĐșŃпДŃĐžĐŒĐ”ĐœŃŃĐČ Đ· ĐŽĐŸŃĐ»ŃĐŽĐ¶Đ”ĐœĐœŃ ŃĐŸĐœĐŸŃŃĐ”ŃĐž ĐœĐ°ŃĐșĐŸĐČĐŸ-ĐŽĐŸŃĐ»ŃĐŽĐœĐŸĐłĐŸ ĐșĐŸĐŒĐżĐ»Đ”ĐșŃŃ ĐœĐ”ĐșĐŸĐłĐ”ŃĐ”ĐœŃĐœĐŸĐłĐŸ ŃĐŸĐ·ŃŃŃĐœĐœŃ. ĐŃĐŸĐČĐ”ĐŽĐ”ĐœĐŸ Đ°ĐœĐ°Đ»ŃĐ· ŃĐŸĐ±ŃŃ ŃŃŃĐ°ŃĐœĐžŃ
Đ°ĐČŃĐŸŃŃĐČ Đ· ĐŒĐ”ŃĐŸŃ ĐżĐŸĐșĐ°Đ·Đ°ŃĐž, ŃĐŸ ĐżŃĐŽĐČĐžŃĐ”ĐœĐœŃ Đ”ŃĐ”ĐșŃĐžĐČĐœĐŸŃŃŃ ŃŃĐœĐșŃŃĐŸĐœŃĐČĐ°ĐœĐœŃ ŃĐžŃŃĐ”ĐŒ ДлДĐșŃŃĐŸĐżĐŸŃŃĐ°ŃĐ°ĐœĐœŃ Ń Đ°ĐșŃŃĐ°Đ»ŃĐœĐŸŃ ĐżŃĐŸĐ±Đ»Đ”ĐŒĐŸŃ ŃŃŃĐ°ŃĐœĐžŃ
ĐŽĐŸŃĐ»ŃĐŽĐ¶Đ”ĐœŃ.This article presents the results of the analysis of the energy consumption modes of the incoherent scattering complex of the Institute of Ionosphere of the National Academy of Sciences and the Ministry of Education and Science of Ukraine to solve the problem of increasing the energy efficiency of a research complex and creating an energy efficient power supply system that will ensure the sustainability of scientific equipment for research programs
of the National Academy of Sciences of Ukraine. The system of power supply of the complex and modes of power consumption of the complex are described. The devices of the radar system are described, as well as the most powerful consumers of electricity, which consume electricity for experimental and economic needs. The energy consumption of the incoherent scattering complex in 2013 is analyzed. Graphs of the average power consumption (daily average) and average power consumption in measurement modes were obtained and presented. The feasibility of work to optimize the energy supply of the research complex of the institute of the ionosphere is described. Possible measures are proposed to reduce the economic cost of conducting experiments on the study of the ionosphere of an incoherent scattering research complex. The analysis of the works of modern authors i s
carried out in order to show that increasing the efficiency of the power supply systems is an actual problem of modern research
Measurement of the branching fraction
The branching fraction is measured in a data sample
corresponding to 0.41 of integrated luminosity collected with the LHCb
detector at the LHC. This channel is sensitive to the penguin contributions
affecting the sin2 measurement from The
time-integrated branching fraction is measured to be . This is the most precise measurement to
date
Model-independent search for CP violation in D0âKâK+ÏâÏ+ and D0âÏâÏ+Ï+Ïâ decays
A search for CP violation in the phase-space structures of D0 and View the MathML source decays to the final states KâK+ÏâÏ+ and ÏâÏ+Ï+Ïâ is presented. The search is carried out with a data set corresponding to an integrated luminosity of 1.0 fbâ1 collected in 2011 by the LHCb experiment in pp collisions at a centre-of-mass energy of 7 TeV. For the KâK+ÏâÏ+ final state, the four-body phase space is divided into 32 bins, each bin with approximately 1800 decays. The p-value under the hypothesis of no CP violation is 9.1%, and in no bin is a CP asymmetry greater than 6.5% observed. The phase space of the ÏâÏ+Ï+Ïâ final state is partitioned into 128 bins, each bin with approximately 2500 decays. The p-value under the hypothesis of no CP violation is 41%, and in no bin is a CP asymmetry greater than 5.5% observed. All results are consistent with the hypothesis of no CP violation at the current sensitivity
Measurement of the CP-violating phase \phi s in Bs->J/\psi\pi+\pi- decays
Measurement of the mixing-induced CP-violating phase phi_s in Bs decays is of
prime importance in probing new physics. Here 7421 +/- 105 signal events from
the dominantly CP-odd final state J/\psi pi+ pi- are selected in 1/fb of pp
collision data collected at sqrt{s} = 7 TeV with the LHCb detector. A
time-dependent fit to the data yields a value of
phi_s=-0.019^{+0.173+0.004}_{-0.174-0.003} rad, consistent with the Standard
Model expectation. No evidence of direct CP violation is found.Comment: 15 pages, 10 figures; minor revisions on May 23, 201
Search for the lepton-flavor-violating decays Bs0âe±Όâ and B0âe±Όâ
A search for the lepton-flavor-violating decays Bs0âe±Όâ and B0âe±Όâ is performed with a data sample, corresponding to an integrated luminosity of 1.0ââfb-1 of pp collisions at âs=7ââTeV, collected by the LHCb experiment. The observed number of Bs0âe±Όâ and B0âe±Όâ candidates is consistent with background expectations. Upper limits on the branching fractions of both decays are determined to be B(Bs0âe±Όâ)101ââTeV/c2 and MLQ(B0âe±Όâ)>126ââTeV/c2 at 95% C.L., and are a factor of 2 higher than the previous bounds
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