The expected busy period for the controllable M/G/1 queueing model operating under the triadic Max (N, T, D) policy is derived by using a new concept so called “the pseudo probability density function.” In order to justify the proposed approaches for the

In submicron MOSFET devices, maintaining the ratio between the channel length (L) and thechannel depth (D) at 3:1 or larger is known to be critical in preventing deleterious short-channel effects. Inthis study, n-type SOI-MOSFETs with a channel length of 0.1µm and a Si film thickness (channel depth) of0.033µm (L:D=3:1) were virtually fabricated using a TSUPREM-4 process simulator. To form functioningtransistors on the very thin Si film, a protective layer of 0.08µm-thick surface oxide was deposited prior tothe source/drain ion implantation so as to dampen the speed of the incoming As ions. The p-type boron dopingconcentration of the Si film, in which the device channel is formed, was used as the key variable in the processsimulation. The finished devices were electrically tested with a Medici device simulator. The result showedthat, for a given channel doping concentration of 1.9~2.5×1018cm−3, the threshold voltage was 0.5~0.7V, andthe subthreshold swing was 70~80mV/dec. These value ranges are all fairly reasonable and should form a‘magic region’ in which SOI-MOSFETs run optimally.

  The expected busy period for the controllable M/G/1 queueing model operating under the triadic policy is derived by using the pseudo probability density function which is totally different from the actual probability density function. In order to justif

TiC-and Ti(C,N)-based cermets are excellent in semi-and final finishing of work piece during cutting operations. Typical microstructure of the cermets is a core/rim structure. The undissolved Ti(C,N) cores contribute to their high hardness while the rim phases, (Ti,M1,M2)(C,N)-type solid solutions, play great roles in enhancing the toughness. In this paper, various ultrafine pre-mixed MeC-Ni powders were synthesized and the powders were sintered or hot pressed after mixing in order to control the size and volume fractions of core and rim phases in the system. This paper will present the factors determining the microstructure along with mechanical properties.

We consider a processing network in which jobs arrive at a fork-node according to a renewal process. Each job requires the completion of two tasks, which are instantaneously assigned by the fork-node to two task-processing nodes that operate like G/M/1 queueing stations. The job is completed when both of two tasks are finished. The sojourn time (or response time) of a job in this G/M/1 fork-join network is the total time it takes to complete the two tasks. Our main result is a closed-form formula for approximating the sojourn-time distribution of a job that arrives in equilibrium. Preliminary results establish the existence and general formulas for the limiting distribution of the task completion times and sojourn times. These formulas, which are not tractable for computations, provide a framework for our approximation based on certain key parameters. Formulas for these parameters are obtained by the use of bounds, properties of D/M/1 and M/M/1 fork-join networks, and exploratory simulations. Statistical tests show that our formulas are good fits for the sojourn-time distributions obtained from simulations.

New Jersey Institute of Technology (NJIT), in collaboration with the University of Hawaii (UH), is upgrading Big Bear Solar Observatory (BBSO) by replacing its principal, 65 cm aperture telescope with a modern, off-axis 1.6 m clear aperture instrument from a 1.7 m blank. The new telescope offers a significant incremental improvement in ground-based infrared and high angular resolution capabilities, and enhances our continuing program to understand photospheric magneto-convection and chromospheric dynamics. These are the drivers for what is broadly called space weather - an important problem, which impacts human technologies and life on earth. This New Solar Telescope (NST) will use the existing BBSO pedestal, pier and observatory building, which will be modified to accept the larger open telescope structure. It will be operated together with our 10 inch (for larger field-of-view vector magnetograms, Ca II K and Ha observations) and Singer-Link (full disk Hα, Ca II K and white light) synoptic telescopes. The NST optical and software control design will be similar to the existing SOLARC (UH) and the planned Advanced Technology Solar Telescope (ATST) facility led by the National Solar Observatory (NSO) - all three are off-axis designs. The NST will be available to guest observers and will continue BBSO's open data policy. The polishing of the primary will be done in partnership with the University of Arizona Mirror Lab, where their proof-of-concept for figuring 8 m pieces of 20 m nighttime telescopes will be the NST's primary mirror. We plan for the NST's first light in late 2005. This new telescope will be the largest aperture solar telescope, and the largest aperture off-axis telescope, located in one of the best observing sites. It will enable new, cutting edge science. The scientific results will be extremely important to space weather and global climate change research.