1,922 research outputs found
Energy-angle dispersion of accelerated heavy ions at 67P/ChuryumovâGerasimenko: implication in the mass-loading mechanism
The Rosetta spacecraft studied the comet 67P/ChuryumovâGerasimenko for nearly two years. The Ion Composition Analyzer instrument on board Rosetta observed the positive ion distributions in the environment of the comet during the mission. A portion of the comet's neutral coma is expected to get ionized, depending on the comet's activity and position relative to the Sun, and the newly created ions are picked up and accelerated by the solar wind electric field, while the solar wind flow is deflected in the opposite direction. This interaction, known as the mass-loading mechanism, was previously studied by comparing the bulk flow direction of both the solar wind protons and the accelerated cometary ions with respect to the direction of the magnetic and the convective solar wind electric field. In this study, we show that energyâangle dispersion is occasionally observed. We report two types of dispersion: one where the observed motion is consistent with ions gyrating in the local magnetic field and another where the energyâangle dispersion is opposite to that expected from gyration in the local magnetic field. Given that the cometary ion gyro-radius in the undisturbed solar wind magnetic and electric field is expected to be too large to be detected in this way, our observations indicate that the local electric field might be significantly smaller than that of the undisturbed solar wind. We also discuss how the energyâangle dispersion, which is not consistent with gyration, may occur due to spatially inhomogeneous densities and electric fields
Investigating short-time-scale variations in cometary ions around comet 67P
The highly varying plasma environment around comet 67P/ChuryumovâGerasimenko inspired an upgrade of the ion mass spectrometer (Rosetta Plasma Consortium Ion Composition Analyzer) with new operation modes, to enable high time resolution measurements of cometary ions. Two modes were implemented, one having a 4 s time resolution in the energy range 0.3â82 eV/q and the other featuring a 1 s time resolution in the energy range 13â50 eV/q. Comparing measurements made with the two modes, it was concluded that 4 s time resolution is enough to capture most of the fast changes of the cometary ion environment. The 1462âh of observations done with the 4 s mode were divided into hour-long sequences. It is possible to sort 84âperâcent of these sequences into one of five categories, depending on their appearance in an energyâtime spectrogram. The ion environment is generally highly dynamic, and variations in ion fluxes and energies are seen on time-scales of 10 s to several minutes
Development of a cometosheath at comet 67P/Churuyumov-Gerasimenko: A case study comparison of Rosetta observations
Context: The ionosphere of a comet is known to deflect the solar wind through
mass loading, but the interaction is dependent on cometary activity. We
investigate the details of this process at comet 67P using the Rosetta Ion
Composition Analyzer. Aims: This study aims to compare the interaction of the
solar wind and cometary ions during two different time periods in the Rosetta
mission. Methods: We compared both the integrated ion moments (density,
velocity, and momentum flux) and the velocity distribution functions for two
days, four months apart. The velocity distribution functions were projected
into a coordinate system dependent on the magnetic field direction and averaged
over three hours. Results: The first case shows highly scattered H+ in both ion
moments and velocity distribution function. The He2+ ions are somewhat
scattered, but less so, and appear more like those of H2O+ pickup ions. The
second case shows characteristic evidence of mass-loading, where the solar wind
species are deflected, but the velocity distribution function is not
significantly changed. Conclusions: The distributions of H+ in the first case,
when compared to He2+ and H2O+ pickup ions, are indicative of a narrow
cometosheath on the scale of the H+ gyroradius. Thus, He2+ and H2O+, with
larger gyroradii, are largely able to pass through this cometosheath. An
examination of the momentum flux tensor suggests that all species in the first
case have a significant non-gyrotropic momentum flux component that is higher
than that of the second mass-loaded case. Mass loading is not a sufficient
explanation for the distribution functions and momentum flux tensor in the
first case, and so we assume this is evidence of bow shock formation.Comment: 14 pages, 9 figures, 3 tables, 2 video
New constraints from Central Chile on the origins of enriched continental compositions in thick-crusted arc magmas
Magmas from continental arcs built on thick crust have elevated incompatible element abundances and âenrichedâ radiogenic isotope ratios compared to magmas erupted in island and continental arcs overlying thinner crust. The relative influence of the slab, mantle, and upper plate on this variability is heavily debated. The Andean Southern Volcanic Zone (SVZ; 33-46° S) is an ideal setting to investigate the production of enriched continental arc compositions, because both crustal thickness and magma chemistry vary coherently along strike. However, the scarcity of primitive magmas in the thick-crusted northern SVZ has hindered
previous regional studies. To better address the origin of enriched continental compositions, we investigate the geochemistry (major and trace element abundances, 87Sr/86Sr and 143Nd/144Nd ratios) of new mafic samples from Don Casimiro and Maipo volcanoes in Diamante-Maipo Caldera Complex of the northern SVZ. While evolved Diamante-Maipo samples show evidence for crustal assimilation, the trace element and
isotopic enrichment of the most mafic samples cannot result from crustal processing, as no known regional or global basement lithologies are enriched in all of the necessary incompatible trace elements. Subduction
erosion models similarly fail to account for the enriched isotopic and trace element signature of these samples. Instead, we suggest that the enrichment of northern SVZ magmas is derived from an enriched ambient mantle component (similar to EM1-type ocean island basalts), superimposed on a northward decline in melt extent. A substantial, but nearly uniform contribution of melts from subducting sediment and altered oceanic crust are required at all latitudes. The EM1-like enrichment may arise from recycling of metasomatized subcontinental lithospheric mantle (M-SCLM), as the isotopic trajectory of primitive rear-arc monogenetic cones trend towards the compositions of SCLM melts sampled across South America. Isotopic data from spatially distributed rear-arc centres demonstrate that the arc-parallel variations in the degree of EM1-type enrichment observed in arc-front samples are also present up to 600 km behind the trench in the rear-arc. Rear-arc trace element systematics require significant but variable quantities of slab melts to be
transported to the mantle wedge at these large trench distances. Overall, we show that a unified model incorporating variable mantle enrichment, slab additions, and melt extents can account for along and acrossarc
trends within the SVZ. The recognition that mantle enrichment plays a key role in the production of enriched continental compositions in the SVZ has important implications for our understanding of the chemical evolution of the Earth. If ambient mantle enrichment is not taken into account, petrogenetic models of evolved lavas may overestimate the role of crustal assimilation, which, in turn, may lead models of
continental crust growth to overestimate the amount of continental material that has been recycled back into the mantle
Pressure and Temperature Effect on Hydrogen Sorption of Carbon Material
The paper presents the experimental results of saturation of the carbon material containing nanotubes with hydrogen from the gas. The dependences of hydrogen concentration from pressure (from 0 to 8 atmospheres), at the same temperature for adsorption (-30 degrees Celsius) and different temperatures for desorption were obtained. The temperature has an influence on sorption-desorption process and sorption properties of carbon material. The amount of residual hydrogen depends on saturation parameters
Influence of the Interplanetary Convective Electric Field on the Distribution of Heavy Pickup Ions Around Mars
This study obtains a statistical representation of 2â15Â keV heavy ions outside of the Martianâinduced magnetosphere and depicts their organization by the solar wind convective electric field (ESW). The overlap in the lifetime of Mars Global Surveyor (MGS) and Mars Express (MEX) provides a period of nearly three years during which magnetometer data from MGS can be used to estimate the direction of ESW in order to better interpret MEX ion data. In this paper we use MGS estimates of ESW to express MEX ion measurements in MarsâSunâElectric field (MSE) coordinates. A new methodological technique used in this study is the limitation of the analysis to a particular instrument mode for which the overlap between proton contamination and plume observations is rare. This allows for confident energetic heavy ion identification outside the induced magnetosphere boundary. On the dayside, we observe high count rates of 2â15Â keV heavy ions more frequently in the +ESW hemisphere (+ZMSE) than in the âESW hemisphere, but on the nightside the reverse asymmetry was found. The results are consistent with planetary origin ions being picked up by the solar wind convective electric field. Though a field of view hole hinders quantification of plume fluxes and velocity space, this new energetic heavy ion identification technique means that Mars Express should prove useful in expanding the time period available to assess general plume loss variation with drivers.Plain Language SummaryThe location and flow direction of oxygen escaping Marsâ atmosphere is organized by a globalâscale electric field associated with the Sunâs flowing magnetic field. While the Mars Express (MEX) satellite is less well equipped than Mars Atmosphere and Volatile Evolution (MAVEN) to estimate exact flux values of ions accelerated by this electric field, our demonstration that MEX can see this population statistically opens a new window of time (preâMAVEN) to studies of the variability of this atmospheric escape channel.Key PointsMars Express heavy ion data outside the magnetic boundary show a statistical asymmetry consistent with other energetic plume studiesThe energetic plume is more prevalent on the dayside (i.e., XÂ >Â 0), while for XÂ <Â 0 higher count rates in the +ESW direction were not seenFor a specific instrument setting, overlap between proton contamination and the plume is rare, allowing for confident plume identificationPeer Reviewedhttps://deepblue.lib.umich.edu/bitstream/2027.42/142551/1/jgra53999.pdfhttps://deepblue.lib.umich.edu/bitstream/2027.42/142551/2/jgra53999_am.pd
Search for the Hypothetical pi -> mu x Decay
The KARMEN collaboration has reported the possible observation of a hitherto
unknown neutral and weakly interacting particle x, which is produced in the
decay pi -> mu + x with a mass m(x) = 33.9 MeV. We have searched for this
hypothetical decay branch by studying muons from pion decay in flight with the
LEPS spectrometer at the piE3 channel at PSI and find branching ratios BR(pi-
to mu- anti-x) < 4e-7 and BR(pi+ to mu+ x) < 7e-8 (95\% C.L.). Together with
the limit BR > 2e-8 derived in a recent theoretical paper our result would
leave only a narrow region for the existence of x if it is a heavy neutrino.Comment: 10 pages, TeX (uses epsf), 3 Postscript figures uu-encode
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