228 research outputs found
Independent Orbiter Assessment (IOA): Analysis of the DPS subsystem
The results of the Independent Orbiter Assessment (IOA) of the Failure Modes and Effects Analysis/Critical Items List (FMEA/CIL) is presented. The IOA approach features a top-down analysis of the hardware to independently determine failure modes, criticality, and potential critical items. The independent analysis results corresponding to the Orbiter Data Processing System (DPS) hardware are documented. The DPS hardware is required for performing critical functions of data acquisition, data manipulation, data display, and data transfer throughout the Orbiter. Specifically, the DPS hardware consists of the following components: Multiplexer/Demultiplexer (MDM); General Purpose Computer (GPC); Multifunction CRT Display System (MCDS); Data Buses and Data Bus Couplers (DBC); Data Bus Isolation Amplifiers (DBIA); Mass Memory Unit (MMU); and Engine Interface Unit (EIU). The IOA analysis process utilized available DPS hardware drawings and schematics for defining hardware assemblies, components, and hardware items. Each level of hardware was evaluated and analyzed for possible failure modes and effects. Criticality was assigned based upon the severity of the effect for each failure mode. Due to the extensive redundancy built into the DPS the number of critical items are few. Those identified resulted from premature operation and erroneous output of the GPCs
Independent Orbiter Assessment (IOA): Analysis of the guidance, navigation, and control subsystem
The results of the Independent Orbiter Assessment (IOA) of the Failure Modes and Effects Analysis (FMEA) and Critical Items List (CIL) is presented. The IOA approach features a top-down analysis of the hardware to determine failure modes, criticality, and potential critical items. To preserve independence, this analysis was accomplished without reliance upon the results contained within the NASA FMEA/CIL documentation. The independent analysis results corresponding to the Orbiter Guidance, Navigation, and Control (GNC) Subsystem hardware are documented. The function of the GNC hardware is to respond to guidance, navigation, and control software commands to effect vehicle control and to provide sensor and controller data to GNC software. Some of the GNC hardware for which failure modes analysis was performed includes: hand controllers; Rudder Pedal Transducer Assembly (RPTA); Speed Brake Thrust Controller (SBTC); Inertial Measurement Unit (IMU); Star Tracker (ST); Crew Optical Alignment Site (COAS); Air Data Transducer Assembly (ADTA); Rate Gyro Assemblies; Accelerometer Assembly (AA); Aerosurface Servo Amplifier (ASA); and Ascent Thrust Vector Control (ATVC). The IOA analysis process utilized available GNC hardware drawings, workbooks, specifications, schematics, and systems briefs for defining hardware assemblies, components, and circuits. Each hardware item was evaluated and analyzed for possible failure modes and effects. Criticality was assigned based upon the severity of the effect for each failure mode
Discovery of a New Deeply Eclipsing SU UMa-Type Dwarf Nova, IY UMa (= TmzV85)
We discovered a new deeply eclipsing SU UMa-type dwarf nova, IY UMa, which
experienced a superoutburst in 2000 January. Our monitoring revealed two
distinct outbursts, which suggest a superoutburst interval of ~800 d, or its
half, and an outburst amplitude of 5.4 mag. From time-series photometry during
the superoutburst, we determined a superhump and orbital period of 0.07588 d
and 0.0739132 d, respectively.Comment: 5 pages, 3 figures, accepted by PASJ lette
HS 2325+8205 - an ideal laboratory for accretion disk physics
We identify HS 2325+8205 as an eclipsing, frequently outbursting dwarf nova
with an orbital period of 279.841731(5) min. Spectroscopic observations are
used to derive the radial velocity curve of the secondary star from absorption
features and also from the H-alpha emission lines, originating from the
accretion disc, yielding K_secondary = K_abs = 237 +- 28 km/s and K_emn = 145
+- 9 km/s respectively. The distance to the system is calculated to be 400
(+200, -140) pc. A photometric monitoring campaign reveals an outburst
recurrence time of 12-14 d, The combination of magnitude range (17-14 mag),
high declination, eclipsing nature and frequency of outbursts makes HS
2325+8205 the ideal system for "real-time" studies of the accretion disc
evolution and behavior in dwarf nova outbursts.Comment: 20 pages, 7 figures. Accepted for Publications of the Astronomical
Society of the Pacifi
Magnetic Reconnection Triggered by the Parker Instability in the Galaxy: Two-Dimensional Numerical Magnetohydrodynamic Simulations and Application to the Origin of X-Ray Gas in the Galactic Halo
We propose the Galactic flare model for the origin of the X-ray gas in the
Galactic halo. For this purpose, we examine the magnetic reconnection triggered
by Parker instability (magnetic buoyancy instability), by performing the
two-dimensional resistive numerical magnetohydrodynamic simulations. As a
result of numerical simulations, the system evolves as following phases: Parker
instability occurs in the Galactic disk. In the nonlinear phase of Parker
instability, the magnetic loop inflates from the Galactic disk into the
Galactic halo, and collides with the anti-parallel magnetic field, so that the
current sheets are created in the Galactic halo. The tearing instability
occurs, and creates the plasmoids (magnetic islands). Just after the plasmoid
ejection, further current-sheet thinning occurs in the sheet, and the anomalous
resistivity sets in. Petschek reconnection starts, and heats the gas quickly in
the Galactic halo. It also creates the slow and fast shock regions in the
Galactic halo. The magnetic field (G), for example, can heat the
gas ( cm) to temperature of K via the
reconnection in the Galactic halo. The gas is accelerated to Alfv\'en velocity
( km s). Such high velocity jets are the evidence of the
Galactic flare model we present in this paper, if the Doppler shift of the
bipolar jet is detected in the Galactic halo. Full size figures are available
at http://www.kwasan.kyoto-u.ac.jp/~tanuma/study/ApJ2002/ApJ2002.htmlComment: 13 pages, 12 figures, uses emulateapj.sty, accepted by Ap
Dynamic interaction of PTP mu with multiple cadherins in vivo
There is a growing body of evidence to implicate reversible tyrosine phosphorylation as an important mechanism in the control of the adhesive function of cadherins. We previously demonstrated that the receptor protein tyrosine phosphatase PTP mu associates with the cadherin-catenin complex in various tissues and cells and, therefore, may be a component of such a regulatory mechanism (Brady-Kalnay, S.M., D.L. Rimm, and N.K. Tonks. 1995. J. Cell Biol. 130:977-986). In this study, we present further characterization of this interaction using a variety of systems. We observed that PTP mu interacted with N-cadherin, E-cadherin, and cadherin-4 (also called R-cadherin) in extracts of rat lung. We observed a direct interaction between PTP mu, and E-cadherin after coexpression in Sf9 cells. In WC5 cells, which express a temperature-sensitive mutant form of v-Src, the complex between PTP mu and E-cadherin was dynamic, and conditions that resulted in tyrosine phosphorylation of E-cadherin were associated with dissociation of PTP mu from the complex. Furthermore, we have demonstrated that the COOH-terminal 38 residues of the cytoplasmic segment of E-cadherin was required for association with PTP mu in WC5 cells. Zondag et al. (Zondag, G., W. Moolenaar, and M. Gebbink. 1996. J. Cell Biol. 134: 1513-1517) have asserted that the association we observed between PTP mu and the cadherin-catenin complex in immunoprecipitates of the phosphatase arises from nonspecific cross-reactivity between BK2, our antibody to PTP mu, and cadherins. In this study we have confirmed our initial observation and demonstrated the presence of cadherin in immunoprecipitates of PTP mu. obtained with three antibodies that recognize distinct epitopes in the phosphatase. In addition, we have demonstrated directly that the anti-PTP mu antibody BK2 that we used initially did not cross-react with cadherin. Our data reinforce the observation of an interaction between PTP mu, and E-cadherin in vitro and in vivo, further emphasizing the potential importance of reversible tyrosine phosphorylation in regulating cadherin function
High-redshift X-ray properties of the haloes of simulated disc galaxies
X-ray luminosities and surface brightness profiles of the hot gas haloes of
simulated disc galaxies at redshifts z=0-2 are presented. The galaxies are
extracted from fully cosmological simulations and correspond in mass to the
Milky Way. We find that the bolometric X-ray luminosities of the haloes
decrease by a factor 4-10 from z~1 to z~0, reflecting the decrease in the rate
at which hot halo gas cools out on to the disc. At all redshifts, most of the
emission is found to originate within 10-15 kpc of the disc. When combined with
models in which the evolution of disc X-ray luminosity is dominated by X-ray
binaries, the predicted halo luminosities at z~1 show good agreement with
constraints from spiral galaxies in Chandra Deep Field data. There is an
indication that haloes with a metal abundance of 0.3 solar overpredict observed
X-ray luminosities at z~1, suggesting that halo metallicities are lower than
this value. Prospects for direct detection of the haloes of Milky Way-sized
galaxies with current and future X-ray instrumentation are discussed. It is
found that XEUS should be able to single out the halo emission of highly
inclined Milky Way-sized disc galaxies out to approximately z=0.3. For such
galaxies in this redshift interval, we estimate a lower limit to the surface
density of detectable haloes on the sky of ~10 deg^(-2). More generally, owing
to their luminosity evolution, the optimum redshifts at which to observe such
haloes could be 0.5<z<1, depending on their assembly history.Comment: 9 pages, 4 figures, minor corrections to conform to version accepted
to MNRA
Two-Dimensional MHD Numerical Simulations of Magnetic Reconnection Triggered by A Supernova Shock in Interstellar Medium, Generation of X-Ray Gas in Galaxy
We examine the magnetic reconnection triggered by a supernova (or a point
explosion) in interstellar medium, by performing two-dimensional resistive
magnetohydrodynamic (MHD) numerical simulations with high spatial resolution.
We found that the magnetic reconnection starts long after a supernova shock
(fast-mode MHD shock) passes a current sheet. The current sheet evolves as
follows: (i) Tearing-mode instability is excited by the supernova shock, and
the current sheet becomes thin in its nonlinear stage. (ii) The current-sheet
thinning is saturated when the current-sheet thickness becomes comparable to
that of Sweet-Parker current sheet. After that, Sweet-Parker type reconnection
starts, and the current-sheet length increases. (iii) ``Secondary tearing-mode
instability'' occurs in the thin Sweet-Parker current sheet. (iv) As a result,
further current-sheet thinning occurs and anomalous resistivity sets in,
because gas density decreases in the current sheet. Petschek type reconnection
starts and heats interstellar gas. Magnetic energy is released quickly while
magnetic islands are moving in the current sheet during Petschek type
reconnection. The released magnetic energy is determined by the interstellar
magnetic field strength, not energy of initial explosion nor distance to
explosion. We suggest that magnetic reconnection is a possible mechanism to
generate X-ray gas in Galaxy.Comment: 17 pages using emulateapj.sty, 24 figures (4colors), submitted to
ApJ, mpeg simulations and psfiles are available at
http://stesun8.stelab.nagoya-u.ac.jp/~tanuma/apj2000/apj2000.htm
Large neutral amino acids in the treatment of PKU: from theory to practice
Notwithstanding the success of the traditional dietary phenylalanine restriction treatment in phenylketonuria (PKU), the use of large neutral amino acid (LNAA) supplementation rather than phenylalanine restriction has been suggested. This treatment modality deserves attention as it might improve cognitive outcome and quality of life in patients with PKU. Following various theories about the pathogenesis of cognitive dysfunction in PKU, LNAA supplementation may have multiple treatment targets: a specific reduction in brain phenylalanine concentrations, a reduction in blood (and consequently brain) phenylalanine concentrations, an increase in brain neurotransmitter concentrations, and an increase in brain essential amino acid concentrations. These treatment targets imply different treatment regimes. This review summarizes the treatment targets and the treatment regimens of LNAA supplementation and discusses the differences in LNAA intake between the classical dietary phenylalanine-restricted diet and several LNAA treatment forms
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