Hardy-type Inequalities On Weighted Orlicz Spaces

This thesis is devoted to the study of integral operators of the form{dollar}{dollar}Kf(x)=\int\sbsp{lcub}0{rcub}{lcub}+\infty{rcub} k(x,t)f(t)dt{dollar}{dollar}on weighted Orlicz spaces. Weight characterizations are obtained for weighted modular inequalities, which generalize the results by Q. Lai and by H. Heinig and L. Maligranda for the Hardy operator. We also give results that parallel those by S. Bloom and R. Kerman for operators with more general kernels, but our results are valid under weaker conditions. Our results also have applications to the Stieltjes transformations and Hardy\u27s inequalities for higher order derivatives.;Furthermore, the results above can be used to characterize the weights for modular inequalities when K is restricted to the monotone functions. These results generalize the corresponding ones in Lebesgue spaces proved by H. Weinig and A. Kufner for the Hardy operators and by V. Stepanov for a class of Volterra convolution operators.;Also, for the identity operator, which is a special case of an integral operator, we study both the modular and norm inequalities.;Finally, a reverse Holder inequality in Orlicz spaces is studied and the result is new even in the Lebesgue space case

Wireless-Connection Drop Prediction, Warning, and Protection

This publication describes systems and techniques directed to wireless-connection drop prediction, warning, and protection. A wireless-communication device, such as a smartphone, includes a wireless-connection manager application. The wireless-communication device, having a wireless connection to an access point of a wireless network, performs operations under the direction of the wireless-connection manager application to predict, warn, and protect a user of instances where the wireless connection may drop. The operations include determining that a quality metric of a signal supporting the wireless connection to the access point does not meet a threshold, determining that another access point to the wireless network is not available, and, in response, presenting a warning to the user to protect the user and allow the user to make decisions so that the wireless-communication device maintains the wireless connection to the access point

Service-Oriented Mobile Network Tracking and Guiding

This publication describes techniques for a User Equipment device (UE) (e.g., a mobile device, a tablet, a wireless-communication device) to guide a user to an area with a requested network service. Mobile device users often encounter situations where the wireless network they are connected to does not provide a requested network service. With no other available means to find a wireless network with the requested network service, users will often wander in attempt to access the network services they desire. Thus, a wireless-connection network manager (WCNM) that can aid the user by guiding them to a physical location where the user previously received access to a requested service is desirable

Magnetostratigraphy of the Lower Triassic beds from Chaohu(China) and its implications for the Induan–Olenekian stage boundary.

A magnetostratigraphic study was performed on the lower 44 m of the West Pingdingshan section near Chaohu city, (Anhui province, China) in order to provide a magnetic polarity scale for the early Triassic. Data from 295 paleomagnetic samples is integrated with a detailed biostratigraphy and lithostratigraphy. The tilt-corrected mean direction from the West Pingdingshan section, passes the reversal and fold tests. The overall mean direction after tilt correction is D=299.9º, I=18.3º (κ=305.2, α95=1.9, N=19). The inferred paleolatitude of the sampling sites (31.6ºN, 117.8ºE) is about 9.4º, consistent with the stable South China block (SCB), though the declinations indicate some 101o counter-clockwise rotations with respect to the stable SCB since the Early Triassic. Low-field anisotropy of magnetic susceptibility indicates evidence of weak strain. The lower part of the Yinkeng Formation is dominated by reversed polarity, with four normal polarity magnetozones (WP2n to WP5n), with evidence of some thinner (<0.5 m thick) normal magnetozones. The continuous magnetostratigraphy from the Yinkeng Formation, provides additional high-resolution details of the polarity pattern through the later parts of the Induan into the lowest Olenekian. The magnetostratigraphic and biostratigraphic data shows the conodont marker for the base of the Olenekian (first presence of Neospathodus waageni) is shortly prior to the base of normal magnetozone WP5n. This provides a secondary marker for mapping the base of the Olenekian into successions without conodonts. This section provides the only well-integrated study from a Tethyan section across this boundary, but problems remain in definitively relating this boundary into Boreal sections with magnetostratigraphy

Studying dawn-dusk asymmetries of Mercury's magnetotail using MHD-EPIC simulations

MESSENGER has observed a lot of dawn-dusk asymmetries in Mercury's magnetotail, such as the asymmetries of the cross-tail current sheet thickness and the occurrence of flux ropes, dipolarization events and energetic electron injections. In order to obtain a global pictures of Mercury's magnetotail dynamics and the relationship between these asymmetries, we perform global simulations with the magnetohydrodynamics with embedded particle-in-cell (MHD-EPIC) model, where Mercury's magnetotail region is covered by a PIC code. Our simulations show that the dawnside current sheet is thicker, the plasma density is larger, and the electron pressure is higher than the duskside. Under a strong IMF driver, the simulated reconnection sites prefer the dawnside. We also found the dipolarization events and the planetward electron jets are moving dawnward while they are moving towards the planet, so that almost all dipolarization events and high-speed plasma flows concentrate in the dawn sector. The simulation results are consistent with MESSENGER observations

Text Data Embedded into a Voice Call

This publication describes systems and techniques directed to embedding text data into a voice call. A first wireless-communication device, such as a smartphone, includes a text-voice manager application. The first wireless-communication device performs the voice call with a second wireless-communication device that includes a peer text-voice manager application. The first wireless-communication device, by executing instructions of the text-voice manager application, performs operations that include receiving text data for a text message, converting the text data to a voice message, detecting silent periods in a stream of a voice transmission, and embedding the voice message into the detected silent periods in the stream of the voice transmission. The second wireless-communication device receives the stream of the voice transmission, detects a pattern in the stream of the voice transmission that indicates a presence of the voice message, de-converts the voice message to the text data, and embeds the text data into a text message displayed on the second wireless-communication device

The role of Stewartson and Ekman layers in turbulent rotating Rayleigh-B\'enard convection

When the classical Rayleigh-B\'enard (RB) system is rotated about its vertical axis roughly three regimes can be identified. In regime I (weak rotation) the large scale circulation (LSC) is the dominant feature of the flow. In regime II (moderate rotation) the LSC is replaced by vertically aligned vortices. Regime III (strong rotation) is characterized by suppression of the vertical velocity fluctuations. Using results from experiments and direct numerical simulations of RB convection for a cell with a diameter-to-height aspect ratio equal to one at $Ra \sim 10^8-10^9$ ($Pr=4-6$) and $0 \lesssim 1/Ro \lesssim 25$ we identified the characteristics of the azimuthal temperature profiles at the sidewall in the different regimes. In regime I the azimuthal wall temperature profile shows a cosine shape and a vertical temperature gradient due to plumes that travel with the LSC close to the sidewall. In regime II and III this cosine profile disappears, but the vertical wall temperature gradient is still observed. It turns out that the vertical wall temperature gradient in regimes II and III has a different origin than that observed in regime I. It is caused by boundary layer dynamics characteristic for rotating flows, which drives a secondary flow that transports hot fluid up the sidewall in the lower part of the container and cold fluid downwards along the sidewall in the top part.Comment: 21 pages, 12 figure

Development of a rotary union for Gifford-McMahon cryocoolers utilized in a 10 MW offshore superconducting wind turbine

Superconducting generators (SCG) show the potential to reduce the head mass of large offshore wind turbines. By evaluating the availability and required cooling capacity in the temperatures range around 20 K, a Gifford-McMahon (GM) cryocooler among all the candidates was selected. The cold head of GM cryocooler is supposed to rotate together with the rotating superconducting coil. However, the scroll compressor of the GM cryocooler must stay stationary due to lubricating oil. As a consequence, a rotary helium union (RHU) utilizing Ferrofluidic® sealing technology was successfully developed to transfer helium gas between the rotating cold head and stationary helium compressor at ambient temperatures. It contains a high-pressure and low-pressure helium path with multiple ports, respectively. Besides the helium line, slip rings with optical fiber channels are also integrated into this RHU to transfer current and measurement signals. With promising preliminary test results, the RHU will be installed in a demonstrator of SCG and further performance investigation will be performed.This research is primarily supported by the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement 308793. Thanks for the technical support from Tom Black and Mark Granoff at Ferrotec

MESSENGER Observations of Fast Plasma Flows in Mercury’s Magnetotail

We present the first observation of fast plasma flows in Mercury’s magnetotail. Mercury experiences substorm activity phenomenologically similar to Earth’s; however, field‐of‐view limitations of the Fast Imaging Plasma Spectrometer (FIPS) prevent the instrument from detecting fast flows in the plasma sheet. Although FIPS measures incomplete plasma distributions, subsonic flows impart an asymmetry on the partial plasma distribution, even if the flow directions are outside the field of view. We combine FIPS observations from 387 intervals containing magnetic field dipolarizations to mitigate these instrument limitations. By taking advantage of variations in spacecraft pointing during these intervals, we construct composite plasma distributions from which mean flows are determined. We find that dipolarizations at Mercury are embedded within fast sunward flows with an averaged speed of ~300 km/s compared to a typical background flow of ~50 km/s.Plain Language SummarySimilar to Earth, Mercury has a global magnetic field that forms a protective cavity, known as the magnetosphere, within the solar wind. The solar wind compresses the dayside magnetosphere, while stretching the nightside magnetosphere behind the planet. Variations within the solar wind cause dynamic activity within Mercury’s magnetosphere, with a process known as magnetic reconnection mediating the interaction. Magnetic reconnection changes the topology of magnetic field lines and transfers energy and momentum from the magnetic field to the plasma within it. At Earth, magnetic reconnection in the nightside magnetosphere drives fast flows of plasma toward the planet, which when nearing the planet are slowed and diverted. These flows cannot be identified directly at Mercury because of limitations of the MESSENGER spacecraft measurements collected there. This research paper develops a new statistical technique to identify and characterize these fast flows at Mercury.Key PointsMultiple FIPS plasma observations from the MESSENGER spacecraft have been combined statistically to determine average flowsObservations collected during dipolarizations produce an average plasma flow of ~300 km/s compared to ~50 km/s during background intervalsSeveral dipolarizations are required to unload Mercury’s magnetotail during a substorm, and some flows may reach the planet’s surfacePeer Reviewedhttps://deepblue.lib.umich.edu/bitstream/2027.42/146314/1/grl58028.pdfhttps://deepblue.lib.umich.edu/bitstream/2027.42/146314/2/grl58028_am.pd