Functional Analysis of the Peroneus Longus and Tibialis Posterior Using Over-Stimulation

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A three-dimensional ring current decay model

This work is an extension of a previous ring current decay model. In the previous work, a two-dimensional kinetic model was constructed to study the temporal variations of the equatorially mirroring ring current ions, considering charge exchange and Coulomb drag losses along drift paths in a magnetic dipole field. In this work, particles with arbitrary pitch angle are considered. By bounce averaging the kinetic equation of the phase space density, information along magnetic field lines can be inferred from the equator. The three-dimensional model is used to simulate the recovery phase of a model great magnetic storm, similar to that which occurred in early February 1986. The initial distribution of ring current ions (at the minimum Dst) is extrapolated to all local times from AMPTE/CCE spacecraft observations on the dawn and dusk sides of the inner magnetosphere spanning the L value range L = 2.25 to 6.75. Observations by AMPTE/CCE of ring current distributions over subsequent orbits during the storm recovery phase are compared to model outputs. In general, the calculated ion fluxes are consistent with observations, except for H+ fluxes at tens of keV, which are always over-estimated. A newly-invented visualization idea, designated as a chromogram, is used to display the spatial and energy dependence of the ring current ion differential flux. Important features of storm-time ring current, such as day-night asymmetry during injection and drift hole on the dayside at low energies (less than 10 keV), are manifested in the chromogram representation. The pitch angle distribution is well fit by the function, j(sub o)(1+Ay(exp n)), where y is sine of the equatorial pitch angle. The evolution of the index n is a combined effect of charge exchange loss and particle drift. At low energies (less than 30 keV), both drift dispersion and charge exchange are important in determining n

Three-dimensional ring current decay model

This work is an extension of a previous ring current decay model. In the previous work, a two-dimensional kinetic model was constructed to study the temporal variations of the equatorially mirroring ring current ions, considering charge exchange and Coulomb drag losses along drift paths in a magnetic dipole field. In this work, particles with arbitrary pitch angle are considered. By bounce averaging the kinetic equation of the phase space density, information along magnetic field lines can be inferred from the equator. The three-dimensional model is used to simulate the recovery phase of a model great magnetic storm, similar to that which occurred in early February 1986. The initial distribution of ring current ions (at the minimum Dst) is extrapolated to all local times from AMPTE/CCE spacecraft observations on the dawnside and duskside of the inner magnetosphere spanning the L value range L = 2.25 to 6.75. Observations by AMPTE/CCE of ring current distributions over subsequent orbits during the storm recovery phase are compared to model outputs. In general, the calculated ion fluxes are consistent with observations, except for H(+) fluxes at tens of keV, which are always overestimated. A newly invented visualization idea, designated as a chromogram, is used to display the spatial and energy dependence of the ring current ion differential flux. Important features of storm time ring current, such as day-night asymmetry during injection and drift hole on the dayside at low energies (less than 10 keV), are manifested in the chromogram representation. The pitch angle distribution is well fit by the function, J(sub o)(1 + Ay(sup n)), where y is sine of the equatorial pitch angle. The evolution of the index n is a combined effect of charge exchange loss and particle drift. At low energies (less than 30 keV), both drift dispersion and charge exchange are important in determining n

Adiabatic energization in the ring current and its relation to other source and loss terms

Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/94822/1/jgra16175.pd

Enhanced NO x in 2006 linked to strong upper stratospheric Arctic vortex

Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/95315/1/grl21996.pd

A bounce‐averaged kinetic model of the ring current ion population

Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/94668/1/grl7966.pd

Plasma properties of superstorms at geosynchronous orbit: How different are they?

Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/94769/1/grl23868.pd

Organisational routines and interfirm collaboration : measurement dilemmas and recommendations for further research steps

Purpose: The paper aims mainly to present the results and consequences of measurement inaccuracies and to make recommendations for further research. Design/Methodology/Approach: We began our research by providing studies on the theoretical origins of constructs in survey questions. Specifically, we studied the theorems and related constructs. We then reviewed the measurement of the constructs, selecting reliable scales. We conducted an initial study on 101 firms in Poland randomly selected from the high-technology sector, specifically the IT sector. We selected an industry in which inter-firm relationships are common. They are distinguished by high innovation, short product and process life cycles and therefor require many relationships to meet customer expectations. The respondents were top managers. The inclusive criterion was their employment of at least five employees. Collected data were analysed with Statistica 13 software (TIBCO Software Inc. (2017). Findings: After solving measurement dilemmas we made methodological recommendations regarding population structure and scales revealing particular constructs. Originality/Value: The implementation of the recommendations aforementioned would allow to formulate and verify hypotheses resulting from the propositions we have formulated while proposing our research framework. Additionally, we obtained a new Propensity to Collaborate scale as the questions referred to particular dimensions joined in quite different groups. Hence, one item has been deleted and the dimensions have been combined. We propose to check the new scale (without dimensions) in the future research.peer-reviewe

Current perceptions on climate change impacts and adaptation for arable crops in Europe

vokKAT. Yksikön huom.: KA

Earth's collision with a solar filament on 21 January 2005: Overview

On 21 January 2005, one of the fastest interplanetary coronal mass ejections (ICME) of solar cycle 23, containing exceptionally dense plasma directly behind the sheath, hit the magnetosphere. We show from charge‐state analysis that this material was a piece of the erupting solar filament and further, based on comparisons to the simulation of a fast CME, that the unusual location of the filament material was a consequence of three processes. As the ICME decelerated, the momentum of the dense filament material caused it to push through the flux rope toward the nose. Diverging nonradial flows in front of the filament moved magnetic flux to the sides of the ICME. At the same time, reconnection between the leading edge of the ICME and the sheath magnetic fields worked to peel away the outer layers of the flux rope creating a remnant flux rope and a trailing region of newly opened magnetic field lines. These processes combined to move the filament material into direct contact with the ICME sheath region. Within 1 h after impact and under northward interplanetary magnetic field (IMF) conditions, a cold dense plasma sheet formed within the magnetosphere from the filament material. Dense plasma sheet material continued to move through the magnetosphere for more than 6 h as the filament passed by the Earth. Densities were high enough to produce strong diamagnetic stretching of the magnetotail despite the northward IMF conditions and low levels of magnetic activity. The disruptions from the filament collision are linked to an array of unusual features throughout the magnetosphere, ionosphere, and atmosphere. These results raise questions about whether rare collisions with solar filaments may, under the right conditions, be a factor in producing even more extreme events. Key Points Study of unusual solar filament evolution and collision with geospace As CME decelerated, filament pushed through flux rope reaching sheath Within 1 h after arrival, cold dense plasma sheet formed from solar filamentPeer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/101865/1/jgra50567.pd