Instruction: what is the prompt that generates the input?

Input: Precise photometric measurements of the upcoming space missions allow thesize, mass, and density of satellites of exoplanets to be determined. Here wepresent such an analysis using the photometric transit timing variation($TTV_p$). We examined the light curve effects of both the transiting planetand its satellite. We define the photometric central time of the transit thatis equivalent to the transit of a fixed photocenter. This point orbits thebarycenter, and leads to the photometric transit timing variations. The exactvalue of $TTV_p$ depends on the ratio of the density, the mass, and the size ofthe satellite and the planet. Since two of those parameters are independent, areliable estimation of the density ratio leads to an estimation of the size andthe mass of the exomoon. Upper estimations of the parameters are possible inthe case when an upper limit of $TTV_p$ is known. In case the density ratiocannot be estimated reliably, we propose an approximation with assuming equaldensities. The presented photocenter $TTV_p$ analysis predicts the size of thesatellite better than the mass. We simulated transits of the Earth-Moon systemin front of the Sun. The estimated size and mass of the Moon are 0.020Earth-mass and 0.274 Earth-size if equal densities are assumed. This result iscomparable to the real values within a factor of 2. If we include the realdensity ratio (about 0.6), the results are 0.010 Earth-Mass and 0.253Earth-size, which agree with the real values within 20%.


Instruction: what is the prompt that generates the input?

Input: A computational model study for complete frequency redistribution linearincoherent two-level atomic radiation trapping in optically dense media usingthe multiple scattering representation is presented. This model study discussat length the influence of the spectral distributions, overall opacity andemission quantum yield to trapping distorted ensemble quantities stressingphysical insight and with a non-specialist audience in mind. Macroscopicreemission yield, lifetime, steady state spectra and spatial distributions arecalculated as a function of intrinsic emission yield, opacity and externalexcitation mode for Doppler, Lorentz and Voigt lineshapes. The work couldconstitute the basis for a final undergraduate or beginning graduate project incomputational physics instruction and implements the analytical developments ofthe previous instalment of this contribution.


Instruction: what is the prompt that generates the input?

Input: We study the influence of cooperative effects such as superradiance andsubradiance, on the scattering properties of dilute atomic gases. We show thatcooperative effects lead to an effective potential between pairs of atoms thatdecays like $1/r$. In the case of superradiance, this potential is attractivefor close enough atoms and can be interpreted as a coherent mesoscopic effect.We consider a model of multiple scattering of a photon among superradiant pairsand calculate the elastic mean free path and the group velocity. We study firstthe case of a scalar wave which allows to obtain and to understand basicfeatures of cooperative effects and multiple scattering. We then turn to thegeneral problem of a vector wave. In both cases, we obtain qualitativelysimilar results and derive, for the case of a scalar wave, analytic expressionsof the elastic mean free path and of the group velocity for an arbitrary (nearresonance) detuning.


Instruction: what is the prompt that generates the input?

Input: The current-voltage (I-V) characteristics of various MgB2 films have beenstudied at different magnetic fields parallel to c-axis. At fields \mu0Hbetween 0 and 5T, vortex liquid-glass transitions were found in the I-Visotherms. Consistently, the I-V curves measured at different temperatures showa scaling behavior in the framework of quasi-two-dimension (quasi-2D) vortexglass theory. However, at \mu0 H >= 5T, a finite dissipation was observed downto the lowest temperature here, T=1.7K, and the I-V isotherms did not scale interms of any known scaling law, of any dimensionality. We suggest that this maybe caused by a mixture of \sigma band vortices and \pi band quasiparticles.Interestingly, the I-V curves at zero magnetic field can still be scaledaccording to the quasi-2D vortex glass formalism, indicating an equivalenteffect of self-field due to persistent current and applied magnetic field.


Instruction: what is the prompt that generates the input?

Input: We present a study of rotation (vsini) and chromospheric activity (Halpha EW)based on an extensive set of high-resolution optical spectra obtained with MIKEon the 6.5m Magellan Clay telescope. Our targets are 74 F-M dwarfs in the youngstellar associations Eta Cha, TW Hydrae, Beta Pic, and Tuc-Hor, spanning agesfrom 6 to 30 Myr. While the Halpha EW for most F and G stars are consistentwith pure photospheric absorption, most K and M stars show chromosphericemission. By comparing Halpha EW in our sample to results in the literature, wesee a clear evolutionary sequence: Chromospheric activity declines steadilyfrom the T Tauri phase to the main sequence. Using activity as an ageindicator, we find a plausible age range for the Tuc-Hor association of 10-40Myr. Between 5 and 30 Myr, we do not see evidence for rotational braking in thetotal sample, thus angular momentum is conserved, in contrast to younger stars.This difference indicates a change in the rotational regulation at 5-10 Myr,possibly because disk braking cannot operate longer than typical disklifetimes, allowing the objects to spin up. The rotation-activity relation isflat in our sample; in contrast to main-sequence stars, there is no linearcorrelation for slow rotators. We argue that this is because young starsgenerate their magnetic fields in a fundamentally different way frommain-sequence stars, and not just the result of a saturated solar-type dynamo.By comparing our rotational velocities with published rotation periods for asubset of stars, we determine ages of 13 (7-20) Myr and 9 (7-17} Myr for theEta Cha and TWA associations, respectively, consistent with previous estimates.Thus we conclude that stellar radii from evolutionary models by Baraffe et al.(1998) are in agreement with the observed radii within +-15%. (abridged)


Instruction: what is the prompt that generates the input?

Input: In this series of three papers we present results from a combinedexperimental and theoretical effort to quantitatively describe capacitivelycoupled radio-frequency discharges in oxygen. The particle-in-cell Monte-Carlomodel on which the theoretical description is based will be described in thepresent paper. It treats space charge fields and transport processes on anequal footing with the most important plasma-chemical reactions. For givenexternal voltage and pressure, the model determines the electric potentialwithin the discharge and the distribution functions for electrons, negativelycharged atomic oxygen, and positively charged molecular oxygen. Previously usedscattering and reaction cross section data are critically assessed and in somecases modified. To validate our model, we compare the densities in the bulk ofthe discharge with experimental data and find good agreement, indicating thatessential aspects of an oxygen discharge are captured.


Instruction: what is the prompt that generates the input?

Input: We study a novel configuration for displacement detection consisting of ananomechanical resonator coupled to both, a radio frequency superconductinginterference device (RF SQUID) and to a superconducting stripline resonator. Weemploy an adiabatic approximation and rotating wave approximation and calculatethe displacement sensitivity. We study the performance of such a displacementdetector when the stripline resonator is driven into a region of nonlinearoscillations. In this region the system exhibits noise squeezing in the outputsignal when homodyne detection is employed for readout. We show thatdisplacement sensitivity of the device in this region may exceed the upperbound imposed upon the sensitivity when operating in the linear region. On theother hand, we find that the high displacement sensitivity is accompanied by aslowing down of the response of the system, resulting in a limited bandwidth.


Instruction: what is the prompt that generates the input?

Input: The Kramers' survival probability has been generalized by using nonextensiveformalism. This nonextensive survival probability is studied in detail andassociated Kramers' rate has been calculated in the high and low viscositylimit. It has been showed that the proportionality of nonextensive Kramers'rate to the nonextensive friction term in the high viscosity limit changes toinverse proportionality in the low viscosity limit. It has also been observedthat friction constant of nonextensive processes is of rescaled form of theordinary frictional term. Since the relation between the ordinary rate andnonextensive rate is found out to be linear, the Arrhenius nature of theKramers' rate is preserved. By using experimental results related to COrebinding to myoglobin after photodissociation, we conclude that nonextensivityplays an important role in protein reactions.


Instruction: what is the prompt that generates the input?

Input: We present a 127deg x 63deg extinction map of the Anticenter of the Galaxy,based on <J-H> and <H-K> colour excess maps from 2MASS. This 8001 square degreemap with a resolution of 4 arcminutes is provided as online material. Thecolour excess ratio <J-H> / <H-K> is used to determine the power law index ofthe reddening law (\beta) for individual regions contained in the area (e.g.Orion, Perseus, Taurus, Auriga, Monoceros, Camelopardalis, Cassiopeia). Onaverage we find a dominant value of \beta=1.8+-0.2 for the individual clouds,in agreement with the canonical value for the interstellar medium. We also showthat there is an internal scatter of \beta values in these regions, and that insome areas more than one dominant \beta value is present. This indicates largescale variations in the dust properties. The analysis of the A_V values withinindividual regions shows a change in the slope of the column densitydistribution with distance. This can either be attributed to a change in thegoverning physical processes in molecular clouds on spatial scales of about 1pcor an A_V dilution with distance in our map.


Instruction: what is the prompt that generates the input?

Input: In this paper we present an upper bound for the decay of correlation for thestationary stochastic process associated with the Entropy Penalized Method. Let$L(x, v):\Tt^n\times\Rr^n\to \Rr$ be a Lagrangian of the form  L(x,v) = {1/2}|v|^2 - U(x) + < P, v>.  For each value of $\epsilon $ and $h$, consider the operator  \Gg[\phi](x):= -\epsilon h {ln}[\int_{\re^N} e^{-\frac{hL(x,v)+\phi(x+hv)}{\epsilon h}}dv], as well as the reversed operator\bar \Gg[\phi](x):= -\epsilon h {ln}[\int_{\re^N}e^{-\frac{hL(x+hv,-v)+\phi(x+hv)}{\epsilon h}}dv], both acting on continuousfunctions $\phi:\Tt^n\to \Rr$. Denote by $\phi_{\epsilon,h} $ the solution of$\Gg[\phi_{\epsilon,h}]=\phi_{\epsilon,h}+\lambda_{\epsilon,h}$, and by $\bar\phi_{\epsilon,h} $ the solution of $\bar \Gg[\phi_{\epsilon,h}]=\bar\phi_{\epsilon,h}+\lambda_{\epsilon,h}$. In order to analyze the decay ofcorrelation for this process we show that the operator $ {\cal L} (\phi) (x) =\int e^{- \frac{h L (x,v)}{\epsilon}} \phi(x+h v) d v,$ has a maximaleigenvalue isolated from the rest of the spectrum.


Instruction: what is the prompt that generates the input?

Input: We report new magnetic field measurements for 14 classical T Tauri stars(CTTSs). We combine these data with one previous field determination in orderto compare our observed field strengths with the field strengths predicted bymagnetospheric accretion models. We use literature data on the stellar mass,radius, rotation period, and disk accretion rate to predict the field strengththat should be present on each of our stars according to these magnetosphericaccretion models. We show that our measured field values do not correlate withthe field strengths predicted by simple magnetospheric accretion theory. Wealso use our field strength measurements and literature X-ray luminosity datato test a recent relationship expressing X-ray luminosity as a function ofsurface magnetic flux derived from various solar feature and main sequence starmeasurements. We find that the T Tauri stars we have observed have weaker thanexpected X-ray emission by over an order of magnitude on average using thisrelationship. We suggest the cause for this is actually a result of the verystrong fields on these stars which decreases the efficiency with which gasmotions in the photosphere can tangle magnetic flux tubes in the corona.


Instruction: what is the prompt that generates the input?

Input: Higher-Order Fixpoint Logic (HFL) is a hybrid of the simply typed\lambda-calculus and the modal \lambda-calculus. This makes it a highlyexpressive temporal logic that is capable of expressing various interestingcorrectness properties of programs that are not expressible in the modal\lambda-calculus.  This paper provides complexity results for its model checking problem. Inparticular we consider those fragments of HFL built by using only types ofbounded order k and arity m. We establish k-fold exponential time completenessfor model checking each such fragment. For the upper bound we use fixpointelimination to obtain reachability games that are singly-exponential in thesize of the formula and k-fold exponential in the size of the underlyingtransition system. These games can be solved in deterministic linear time. As asimple consequence, we obtain an exponential time upper bound on the expressioncomplexity of each such fragment.  The lower bound is established by a reduction from the word problem foralternating (k-1)-fold exponential space bounded Turing Machines. Since thereare fixed machines of that type whose word problems are already hard withrespect to k-fold exponential time, we obtain, as a corollary, k-foldexponential time completeness for the data complexity of our fragments of HFL,provided m exceeds 3. This also yields a hierarchy result in expressive power.


Instruction: what is the prompt that generates the input?

Input: Owing to their distinct properties, carbon nanotubes (CNTs) have emerged aspromising candidate for field emission devices. It has been foundexperimentally that the results related to the field emission performance showvariability. The design of an efficient field emitting device requires theanalysis of the variabilities with a systematic and multiphysics based modelingapproach. In this paper, we develop a model of randomly oriented CNTs in a thinfilm by coupling the field emission phenomena, the electron-phonon transportand the mechanics of single isolated CNT. A computational scheme is developedby which the states of CNTs are updated in time incremental manner. The devicecurrent is calculated by using Fowler-Nordheim equation for field emission tostudy the performance at the device scale.


Instruction: what is the prompt that generates the input?

Input: We differentiate between the metal enrichment of the gas in virializedminihalos and that of the intergalactic medium at high redshift, pertinent tocosmological reionization, with the initial expectation that gas in the highdensity regions within formed dark matter halos may be more robust thusresistant to mixing with lower density intergalactic medium. Using detailedhydrodynamic simulations of gas clouds in minihalos subject to destructiveprocesses associated with the encompassing intergalactic shocks carryingmetal-enriched gas, we find, as an example, that, for realistic shocks ofvelocities of 10-100km/s, more than (90%,65%) of the high density gas withrho>500 rhob inside a minihalo virialized at z=10 of mass (10^7,10^6)Msunremains at a metallicity lower than 3% of that of the intergalactic medium byredshift z=6. It may be expected that the high density gas in minihalos becomesfuel for subsequent star formation, when they are incorporated into largerhalos where efficient atomic cooling can induce gas condensation hence starformation. Since minihalos virialize at high redshift when the universe is notexpected to have been significantly reionized, the implication is that gas invirialized minihalos may provide an abundant reservoir of primordial gas topossibly allow for the formation of Population-III metal-free stars to extendto much lower redshift than otherwise expected based on the enrichment ofintergalactic medium.


Instruction: what is the prompt that generates the input?

Input: The rotor-router model is a deterministic analogue of random walk. It can beused to define a deterministic growth model analogous to internal DLA. We showthat the set of occupied sites for this model on an infinite regular tree is aperfect ball whenever it can be, provided the initial rotor configuration isacyclic (that is, no two neighboring vertices have rotors pointing to oneanother). This is proved by defining the rotor-router group of a graph, whichwe show is isomorphic to the sandpile group. We also address the question ofrecurrence and transience: We give two rotor configurations on the infiniteternary tree, one for which chips exactly alternate escaping to infinity withreturning to the origin, and one for which every chip returns to the origin.Further, we characterize the possible "escape sequences" for the ternary tree,that is, binary words a_1 ... a_n for which there exists a rotor configurationso that the k-th chip escapes to infinity if and only if a_k=1.


Instruction: what is the prompt that generates the input?

Input: We have performed self-consistent 2.5-dimensional nonsteady MHD numericalsimulations of jet formation as long as possible, including the dynamics ofaccretion disks. Although the previous nonsteady MHD simulations forastrophysical jets revealed that the characteristics of nonsteady jets aresimilar to those of steady jets, the calculation time of these simulations isvery short compared with the time scale of observed jets. Thus we haveinvestigated long term evolutions of mass accretion rate, mass outflow rate,jet velocity, and various energy flux. We found that the ejection of jet isquasi-periodic. The period of the ejection is related to the time needed forthe initial magnetic filed to be twisted to generate toroidal filed. We compareour results with both the steady state theory and previous 2.5-dimensionalnonsteady MHD simulations.


Instruction: what is the prompt that generates the input?

Input: In this two-part paper, we consider the multiantenna multihop relay channelsin which the source signal arrives at the destination through N independentrelaying hops in series. The main concern of this work is to design relayingstrategies that utilize efficiently the relays in such a way that the diversityis maximized. In part I, we focus on the amplify-and-forward (AF) strategy withwhich the relays simply scale the received signal and retransmit it. Morespecifically, we characterize the diversity-multiplexing tradeoff (DMT) of theAF scheme in a general multihop channel with arbitrary number of antennas andarbitrary number of hops. The DMT is in closed-form expression as a function ofthe number of antennas at each node. First, we provide some basic results onthe DMT of the general Rayleigh product channels. It turns out that theseresults have very simple and intuitive interpretation. Then, the results areapplied to the AF multihop channels which is shown to be equivalent to theRayleigh product channel, in the DMT sense. Finally, the project-and-forward(PF) scheme, a variant of the AF scheme, is proposed. We show that the PFscheme has the same DMT as the AF scheme, while the PF can have significantpower gain over the AF scheme in some cases. In part II, we will derive theupper bound on the diversity of the multihop channels and show that it can beachieved by partitioning the multihop channel into AF subchannels.


Instruction: what is the prompt that generates the input?

Input: Gravitational waves from the inspiral and coalescence of supermassiveblack-hole (SMBH) binaries with masses ~10^6 Msun are likely to be among thestrongest sources for the Laser Interferometer Space Antenna (LISA). Wedescribe a three-stage data-analysis pipeline designed to search for andmeasure the parameters of SMBH binaries in LISA data. The first stage uses atime-frequency track-search method to search for inspiral signals and provide acoarse estimate of the black-hole masses m_1, m_2 and of the coalescence timeof the binary t_c. The second stage uses a sequence of matched-filter templatebanks, seeded by the first stage, to improve the measurement accuracy of themasses and coalescence time. Finally, a Markov Chain Monte Carlo search is usedto estimate all nine physical parameters of the binary. Using results from thesecond stage substantially shortens the Markov Chain burn-in time and allows usto determine the number of SMBH-binary signals in the data before startingparameter estimation. We demonstrate our analysis pipeline using simulated datafrom the first LISA Mock Data Challenge. We discuss our plan for improving thispipeline and the challenges that will be faced in real LISA data analysis.


Instruction: what is the prompt that generates the input?

Input: We replace the ice Ansatz on matrix solutions of the Yang-Baxter equation bya weaker condition which we call "rime". Rime solutions include the standardDrinfeld-Jimbo R-matrix. Solutions of the Yang--Baxter equation within the rimeAnsatz which are maximally different from the standard one we call "strictrime". A strict rime non-unitary solution is parameterized by a projectivevector. We show that this solution transforms to the Cremmer-Gervais R-matrixby a change of basis with a matrix containing symmetric functions in thecomponents of the parameterizing vector. A strict unitary solution (the rimeAnsatz is well adapted for taking a unitary limit) is shown to be equivalent toa quantization of a classical "boundary" r-matrix of Gerstenhaber andGiaquinto. We analyze the structure of the elementary rime blocks and find, asa by-product, that all non-standard R-matrices of GL(1|1)-type can be uniformlydescribed in a rime form.  We discuss then connections of the classical rime solutions with the Bezoutoperators. The Bezout operators satisfy the (non-)homogeneous associativeclassical Yang--Baxter equation which is related to the Rota-Baxter operators.  We classify the rime Poisson brackets: they form a 3-dimensional pencil. Anormal form of each individual member of the pencil depends on the discriminantof a certain quadratic polynomial. We also classify orderable quadratic rimeassociative algebras.  For the standard Drinfeld-Jimbo solution, there is a choice of themultiparameters, for which it can be non-trivially rimed. However, not everyBelavin-Drinfeld triple admits a choice of the multiparameters for which it canbe rimed. We give a minimal example.


Instruction: what is the prompt that generates the input?

Input: We perform a comprehensive analysis of the Minimal Supersymmetric StandardModel (MSSM) in the scenario where the scalar partners of the fermions and theHiggs particles (except for the Standard-Model-like one) are assumed to be veryheavy and are removed from the low-energy spectrum. We first summarize ourdetermination of the mass spectrum, in which we include the one-loop radiativecorrections and resum to all orders the leading logarithms of the large scalarmasses, and describe the implementation of these features in the FORTRAN codeSuSpect which calculates the masses and couplings of the MSSM particles. Wethen study in detail the phenomenology of the model in scenarios where thegaugino mass parameters are non-universal at the GUT scale, which leads to veryinteresting features that are not present in the widely studied case ofuniversal gaugino mass parameters. We discuss the constraints from collidersearches and high-precision measurements, the cosmological constraints on therelic abundance of the neutralino candidate for the Dark Matter in the Universe- where new and interesting channels for neutralino annihilation appear - andthe gluino lifetime. We then analyze, in the case of non-universal gauginomasses, the decays of the Higgs boson (in particular decays into andcontributions of SUSY particles), of charginos and neutralinos (in particulardecays into Higgs bosons and photons) and of gluinos, and highlight thedifferences from the case of universal gaugino masses.


Instruction: what is the prompt that generates the input?

Input: We present a search for the near infrared spectroscopic signature of theclose orbiting extrasolar giant planet HD 75289b. We obtained ~230 spectra inthe wavelength range 2.18 - 2.19 microns using the Phoenix spectrograph atGemini South. By considering the direct spectrum, derived from irradiated modelatmospheres, we search for the absorption profile signature present in thecombined star and planet light. Since the planetary spectrum is separated fromthe stellar spectrum at most phases, we apply a phase dependent orbital modeland tomographic techniques to search for absorption signatures.  Because the absorption signature lies buried in the noise of a singleexposure we apply a multiline deconvolution to the spectral lines available inorder to boost the effective S/N ratio of the data. The wavelength coverage of80 angstroms is expected to contain ~100 planetary lines, enabling a mean linewith S/N ratio of ~800 to be achieved after deconvolution. We are neverthelessunable to detect the presence of the planet in the data and carry out furthersimulations to show that broader wavelength coverage should enable a planetlike HD 75289b to be detected with 99.9 per cent (4 sigma) confidence. Weinvestigate the sensitivity of our method and estimate detection tolerances formismatches between observed and model planetary atmospheres.


Instruction: what is the prompt that generates the input?

Input: We characterize the dynamical behavior of continuous-time, Markovian quantumsystems with respect to a subsystem of interest. Markovian dynamics describes awide class of open quantum systems of relevance to quantum informationprocessing, subsystem encodings offering a general pathway to faithfullyrepresent quantum information. We provide explicit linear-algebraiccharacterizations of the notion of invariant and noiseless subsystem forMarkovian master equations, under different robustness assumptions formodel-parameter and initial-state variations. The stronger concept of anattractive quantum subsystem is introduced, and sufficient existence conditionsare identified based on Lyapunov's stability techniques. As a main controlapplication, we address the potential of output-feedback Markovian controlstrategies for quantum pure state-stabilization and noiseless-subspacegeneration. In particular, explicit results for the synthesis of stabilizingsemigroups and noiseless subspaces in finite-dimensional Markovian systems areobtained.


Instruction: what is the prompt that generates the input?

Input: The interference channel with degraded message sets (IC-DMS) refers to acommunication model in which two senders attempt to communicate with theirrespective receivers simultaneously through a common medium, and one of thesenders has complete and a priori (non-causal) knowledge about the messagebeing transmitted by the other. A coding scheme that collectively hasadvantages of cooperative coding, collaborative coding, and dirty paper coding,is developed for such a channel. With resorting to this coding scheme,achievable rate regions of the IC-DMS in both discrete memoryless and Gaussiancases are derived, which, in general, include several previously known rateregions. Numerical examples for the Gaussian case demonstrate that in thehigh-interference-gain regime, the derived achievable rate regions offerconsiderable improvements over these existing results.


Instruction: what is the prompt that generates the input?

Input: We follow the changes in the structure of the accretion disk of the dwarfnova V2051 Oph along two separate outbursts in order to investigate the causesof its recurrent outbursts. We apply eclipse mapping techniques to a set oflight curves covering a normal (July 2000) and a low-amplitude (August 2002)outburst to derive maps of the disk surface brightness distribution atdifferent phases along the outburst cycles. The sequence of eclipse maps of the2000 July outburst reveal that the disk shrinks at outburst onset while anuneclipsed component of 13 per cent of the total light develops. The derivedradial intensity distributions suggest the presence of an outward-movingheating wave during rise and of an inward-moving cooling wave during decline.The inferred speed of the outward-moving heating wave is ~ 1.6 km/s, while thespeed of the cooling wave is a fraction of that. A comparison of the measuredcooling wave velocity on consecutive nights indicates that the cooling waveaccelerates as it travels towards disk center, in contradiction with theprediction of the disk instability model. From the inferred speed of theheating wave we derive a viscosity parameter alpha_{hot} ~ 0.13, comparable tothe measured viscosity parameter in quiescence. The 2002 August outburst hadlower amplitude (\Delta B ~ 0.8 mag) and the disk at outburst maximum wassmaller than on 2000 July. For an assumed distance of 92 pc, we find that alongboth outbursts the disk brightness temperatures remain below the minimumexpected according to the disk instability model. The results suggest that theoutbursts of V2051 Oph are caused by bursts of increased mass transfer from themass-donor star.


Instruction: what is the prompt that generates the input?

Input: We estimate the spin relaxation rate due to spin-orbit coupling and acousticphonon scattering in weakly-confined quantum dots with up to five interactingelectrons. The Full Configuration Interaction approach is used to account forthe inter-electron repulsion, and Rashba and Dresselhaus spin-orbit couplingsare exactly diagonalized. We show that electron-electron interaction stronglyaffects spin-orbit admixture in the sample. Consequently, relaxation ratesstrongly depend on the number of carriers confined in the dot. We identify themechanisms which may lead to improved spin stability in few electron (>2)quantum dots as compared to the usual one and two electron devices. Finally, wediscuss recent experiments on triplet-singlet transitions in GaAs dots subjectto external magnetic fields. Our simulations are in good agreement with theexperimental findings, and support the interpretation of the observed spinrelaxation as being due to spin-orbit coupling assisted by acoustic phononemission.


Instruction: what is the prompt that generates the input?

Input: We present multi-wavelength optical and infrared photometry of 170 previouslyknown low mass stars and brown dwarfs of the 5 Myr Collinder 69 cluster (LambdaOrionis). The new photometry supports cluster membership for most of them, withless than 15% of the previous candidates identified as probable non-members.The near infrared photometry allows us to identify stars with IR excesses, andwe find that the Class II population is very large, around 25% for stars (inthe spectral range M0 - M6.5) and 40% for brown dwarfs, down to 0.04 Msun,despite the fact that the H(alpha) equivalent width is low for a significantfraction of them. In addition, there are a number of substellar objects,classified as Class III, that have optically thin disks. The Class II membersare distributed in an inhomogeneous way, lying preferentially in a filamentrunning toward the south-east. The IR excesses for the Collinder 69 membersrange from pure Class II (flat or nearly flat spectra longward of 1 micron), totransition disks with no near-IR excess but excesses beginning within the IRACwavelength range, to two stars with excess only detected at 24 micron.Collinder 69 thus appears to be at an age where it provides a naturallaboratory for the study of primordial disks and their dissipation.


Instruction: what is the prompt that generates the input?

Input: We study the thermal interaction between two nearby thin metallic wires, atfinite temperature. It is shown that the Johnson currents in the wires giverise, via inductive coupling, to a repulsive force between them. This thermalinteraction exhibits all the puzzling features found recently in the thermalCasimir effect for lossy metallic plates, suggesting that the physical originof the difficulties encountered in the Casimir problem resides in the inductivecoupling between the Johnson currents inside the plates. We show that in oursimple model all puzzles are resolved if account is taken of capacitive effectsassociated with the end points of the wires. Our findings suggest thatcapacitive finite-size effects may play an important role in the resolution ofthe analogous problems met in the thermal Casimir effect.


Instruction: what is the prompt that generates the input?

Input: We introduce VErsatile SPectral Analysis (VESPA): a new method which aims torecover robust star formation and metallicity histories from galactic spectra.VESPA uses the full spectral range to construct a galaxy history from syntheticmodels. We investigate the use of an adaptative parametrization grid to recoverreliable star formation histories on a galaxy-by-galaxy basis. Our goal isrobustness as opposed to high resolution histories, and the method is designedto return high time resolution only where the data demand it. In this paper wedetail the method and we present our findings when we apply VESPA to syntheticand real Sloan Digital Sky Survey (SDSS) spectroscopic data. We show that thenumber of parameters that can be recovered from a spectrum depends strongly onthe signal-to-noise, wavelength coverage and presence or absence of a youngpopulation. For a typical SDSS sample of galaxies, we can normally recoverbetween 2 to 5 stellar populations. We find very good agreement between VESPAand our previous analysis of the SDSS sample with MOPED.


Instruction: what is the prompt that generates the input?

Input: The magnetoelectric behavior of BiFeO$_3$ has been explored on the basis ofaccurate density functional calculations. The structural, electronic, magnetic,and ferroelectric properties of BiFeO$_3$ are predicted correctly withoutincluding strong correlation effect in the calculation. Moreover, theexperimentally-observed elongation of cubic perovskite-like lattice along the[111] direction is correctly reproduced. At high pressure we predicted apressure-induced structural transition and the total energy calculations atexpanded lattice show two lower energy ferroelectric phases, closer in energyto the ground state phase. Band-structure calculations show that BiFeO$_3$ willbe an insulator in A- and G-type antiferromagnetic phases and a metal in othermagnetic configurations. Chemical bonding in BiFeO$_3$ has been analyzed usingvarious tools and electron localization function analysis shows thatstereochemically active lone-pair electrons at the Bi sites are responsible fordisplacements of the Bi atoms from the centro-symmetric to thenoncentrosymmetric structure and hence the ferroelectricity. A largeferroelectric polarization (88.7 $\mu$C/cm$^{2}$) is predicted in accordancewith recent experimental findings. The net polarization is found to mainly ($>$98%) originate from Bi atoms. Moreover the large scatter in experimentallyreported polarization values is due to the large anisotropy in the spontaneouspolarization.


Instruction: what is the prompt that generates the input?

Input: Previously, we have identified the cytoplasmic zinc metalloproteaseinsulin-degrading enzyme(IDE) in human tissues by an immunohistochemical methodinvolving no antigen retrieval (AR) by pressure cooking to avoid artifacts byendogenous biotin exposure and a detection kit based on the labeledstreptavidin biotin (LSAB) method. Thereby, we also employed 3% hydrogenperoxide(H2O2) for the inhibition of endogenous peroxidase activity andincubated the tissue sections with the biotinylated secondary antibody at roomtemperature (RT). We now add the immunohistochemical details that had led us tothis optimized procedure as they also bear a more general relevance whendemonstrating intracellular tissue antigens. Our most important result is thatendogenous peroxidase inhibition by 0.3% H2O2 coincided with an apparentlypositive IDE staining in an investigated breast cancer specimen whereascombining a block by 3% H2O2 with an incubation of the biotinylated secondaryantibody at RT, yet not at 37 degrees Celsius, revealed this specimen as almostentirely IDE-negative. Our present data caution against three differentimmunohistochemical pitfalls that might cause falsely positive results andartifacts when using an LSAB- and peroxidase-based detection method: pressurecooking for AR, insufficient quenching of endogenous peroxidases and heating oftissue sections while incubating with biotinylated secondary antibodies.


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Input: We present a local interpretation of what is usually considered to be anonlocal de Broglie-Bohm trajectory prescription for an entangled singlet stateof massive particles. After reviewing various meanings of the term``nonlocal'', we show that by using appropriately retarded wavefunctions (i.e.,the locality loophole) this local model can violate Bell's inequality, withoutmaking any appeal to detector inefficiencies.  We analyze a possible experimental configuration appropriate to massivetwo-particle singlet wavefunctions and find that as long as the particles arenot ultra-relativistic, a locality loophole exists and Dirac wave(s) canpropagate from Alice or Bob's changing magnetic field, through space, to theother detector, arriving before the particle and thereby allowing a localinterpretation to the 2-particle de Broglie-Bohm trajectories.  We also propose a physical effect due to changing magnetic fields in aStern-Gerlach EPR setup that will throw away events and create a detectorloophole in otherwise perfectly efficient detectors, an effect that is onlysignificant for near-luminal particles that might otherwise close the localityloophole.


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Input: Aims: In the context of space interferometry missions devoted to the searchof exo-Earths, this paper investigates the capabilities of new single modeconductive waveguides at providing modal filtering in an infrared andmonochromatic nulling experiment; Methods: A Michelson laser interferometerwith a co-axial beam combination scheme at 10.6 microns is used. Afterintroducing a Pi phase shift using a translating mirror, dynamic and staticmeasurements of the nulling ratio are performed in the two cases where modalfiltering is implemented and suppressed. No additional active control of thewavefront errors is involved. Results: We achieve on average a statisticalnulling ratio of 2.5e-4 with a 1-sigma upper limit of 6e-4, while a best nullof 5.6e-5 is obtained in static mode. At the moment, the impact of externalvibrations limits our ability to maintain the null to 10 to 20 seconds.;Conclusions: A positive effect of SM conductive waveguide on modal filteringhas been observed in this study. Further improvement of the null should bepossible with proper mechanical isolation of the setup.


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Input: We have performed a simulation study of Langmuir turbulence in the Earth'sionosphere by means of a Zakharov model with parameters relevant for the Flayer. The model includes dissipative terms to model collisions and Landaudamping of the electrons and ions, and a linear density profile, which modelsthe ionospheric plasma inhomogeneity whose length scale is of the order 10--100km. The injection of energy into the system is modeled by a constant sourceterm in the Zakharov equation. Langmuir turbulence is excited ``on-demand'' incontrolled ionospheric modification experiments where the energy is provided byan HF radio beam injected into the overhead ionospheric plasma. The ensuingturbulence can be studied with radars and in the form of secondary radiationrecorded by ground-based receivers. We have analyzed spectral signatures of theturbulence for different sets of parameters and different altitudes relative tothe turning point of the linear Langmuir mode where the Langmuir frequencyequals the local plasma frequency. By a parametric analysis, we have derived asimple scaling law, which links the spectral width of the turbulent frequencyspectrum to the physical parameters in the ionosphere. The scaling law providesa quantitative relation between the physical parameters (temperatures, electronnumber density, ionospheric length scale, etc.) and the observed frequencyspectrum. This law may be useful for interpreting experimental results.


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Input: Parity doubling in excited hadrons is reviewed. Parity degeneracy in hadronswas first experimentally observed 40 years ago. Recently new experimental dataon light mesons caused much excitement and renewed interest to the phenomenon,which still remains to be enigmatic. The present retrospective review is anattempt to trace the history of parity doubling phenomenon, thus providing akind of introduction to the subject. We begin with early approaches of 1960s(Regge theory and dynamical symmetries) and end up with the latest trends(manifestations of broader degeneracies and AdS/QCD). We show the evolution ofvarious ideas about parity doubling. The experimental evidence for thisphenomenon is scrutinized in the non-strange sector. Some experiments of 1960sdevoted to the search for missing non-strange bosons are re-examined and it isargued that results of these experiments are encouraging from the modernperspective.


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Input: Aims: We aim at estimating the spectral energy distributions (SEDs) and thephysical parameters related to the black holes harbored in eight highX-ray-to-optical (F_X/F_R>10) obscured quasars at z>0.9 selected in the 2--10keV band from the HELLAS2XMM survey.  Methods: We use IRAC and MIPS 24 micron observations, along with optical andKs-band photometry, to obtain the SEDs of the sources. The observed SEDs aremodeled using a combination of an elliptical template and torus emission (usingthe phenomenological templates of Silva et al. 2004) for six sources associatedwith passive galaxies; for two point-like sources, the empirical SEDs of redquasars are adopted. The bolometric luminosities and the M_BH-L_K relation areused to provide an estimate of the masses and Eddington ratios of the blackholes residing in these AGN.  Results: All of our sources are detected in the IRAC and MIPS (at 24 micron)bands. The SED modeling described above is in good agreement with the observednear- and mid-infrared data. The derived bolometric luminosities are in therange ~10^45-10^47 erg s^-1, and the median 2--10 keV bolometric correction is~25, consistent with the widely adopted value derived by Elvis et al. (1994).For the objects with elliptical-like profiles in the K_s band, we derive highstellar masses (0.8-6.2)X10^11 Mo, black hole masses in the range(0.2-2.5)X10^9 Mo, and Eddington ratios L/L_Edd<0.1, suggesting a low-accretionphase.


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Input: To examine the evolution of giant molecular clouds in the stream of a hotplasma we performed two-dimensional hydrodynamical simulations that take fullaccount of self-gravity, heating and cooling effects and heat conduction byelectrons. We use the thermal conductivity of a fully ionized hydrogen plasmaproposed by Spitzer and a saturated heat flux according to Cowie & McKee inregions where the mean free path of the electrons is large compared to thetemperature scaleheight. Significant structural and evolutionary differencesoccur between simulations with and without heat conduction. Dense clouds inpure dynamical models experience dynamical destruction by Kelvin-Helmholtz (KH)instability. In static models heat conduction leads to evaporation of suchclouds. Heat conduction acting on clouds in a gas stream smooths out steeptemperature and density gradients at the edge of the cloud because theconduction timescale is shorter than the cooling timescale. This diminishes thevelocity gradient between the streaming plasma and the cloud, so that thetimescale for the onset of KH instabilities increases, and the surface of thecloud becomes less susceptible to KH instabilities. The stabilisation effect ofheat conduction against KH instability is more pronounced for smaller and lessmassive clouds. As in the static case more realistic cloud conditions allowheat conduction to transfer hot material onto the cloud's surface and to mixthe accreted gas deeper into the cloud.


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Input: We study resonances of multidimensional chaotic map dynamics. We use thecalculus of variations to determine the additive forcing function that inducesthe largest response, that is, the greatest deviation from the unperturbeddynamics. We include the additional constraint that only select degrees offreedom be forced, corresponding to a very general class of problems in whichnot all of the degrees of freedom in an experimental system are accessible toforcing. We find that certain Lagrange multipliers take on a fundamentalphysical role as the efficiency of the forcing function and the effectiveforcing experienced by the degrees of freedom which are not forced directly.Furthermore, we find that the product of the displacement of nearbytrajectories and the effective total forcing function is a conserved quantity.We demonstrate the efficacy of this methodology with several examples.


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Input: The magnetic and thermodynamic properties of spin-1/2 Heisenberg diamondchains are investigated in three different cases: (a) J1, J2, J3>0(frustrated); (b) J1, J3<0, J2>0 (frustrated); and (c) J1, J2>0, J3<0(non-frustrated). The density matrix renormalization group (DMRG) technique isinvoked to study the properties of the system in the ground state, while thetransfer matrix renormalization group (TMRG) technique is applied to explorethe thermodynamic properties. The local magnetic moments, spin correlationfunctions, and static structure factors are discussed in the ground state forthe three cases. It is shown that the static structure factor S(q) shows peaksat wavevectors $q=a\pi /3$ (a=0,1,2,3,4,5) for different couplings in a zeromagnetic field, which, however in the magnetic fields where the magnetizationplateau with m=1/6 pertains, exhibits the peaks only at q=0, $2\pi /3$ and$4\pi /3$, which are found to be couplings-independent. The DMRG results of thezero-field static structure factor can be nicely fitted by a linearsuperposition of six modes, where two fitting equations are proposed. It isobserved that the six modes are closely related to the low-lying excitations ofthe system. At finite temperatures, the double-peak structures of thesusceptibility and specific heat against temperature are obtained, where thepeak positions and heights are found to depend on the competition of thecouplings. It is also uncovered that the XXZ anisotropy of F and AF couplingsleads the system of case (c) to display quite different behaviors. In addition,the experimental data of the susceptibility, specific heat and magnetizationfor the compound Cu$_{3}$(CO$_{3}$)$_{2}$(OH)$_{2}$ are fairly compared withour TMRG results.


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Input: Motivation: Profile hidden Markov Models (pHMMs) are a popular and veryuseful tool in the detection of the remote homologue protein families.Unfortunately, their performance is not always satisfactory when proteins arein the 'twilight zone'. We present HMMER-STRUCT, a model construction algorithmand tool that tries to improve pHMM performance by using structural informationwhile training pHMMs. As a first step, HMMER-STRUCT constructs a set of pHMMs.Each pHMM is constructed by weighting each residue in an aligned proteinaccording to a specific structural property of the residue. Properties usedwere primary, secondary and tertiary structures, accessibility and packing.HMMER-STRUCT then prioritizes the results by voting. Results: We used the SCOPdatabase to perform our experiments. Throughout, we apply leave-one-family-outcross-validation over protein superfamilies. First, we used the MAMMOTH-multstructural aligner to align the training set proteins. Then, we performed twosets of experiments. In a first experiment, we compared structure weightedmodels against standard pHMMs and against each other. In a second experiment,we compared the voting model against individual pHMMs. We compare methodperformance through ROC curves and through Precision/Recall curves, and assesssignificance through the paired two tailed t-test. Our results show significantperformance improvements of all structurally weighted models over defaultHMMER, and a significant improvement in sensitivity of the combined models overboth the original model and the structurally weighted models.


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Input: I review the status of science with wide field surveys. For many decadessurveys have been the backbone of astronomy, and the main engine of discovery,as we have mapped the sky at every possible wavelength. Surveys are anefficient use of resources. They are important as a fundamental resource; tomap intrinsically large structures; to gain the necessary statistics to addresssome problems; and to find very rare objects. I summarise major recent widefield surveys - 2MASS, SDSS, 2dfGRS, and UKIDSS - and look at examples of theexciting science they have produced, covering the structure of the Milky Way,the measurement of cosmological parameters, the creation of a new fieldstudying substellar objects, and the ionisation history of the Universe. I thenlook briefly at upcoming projects in the optical-IR survey arena - VISTA,PanSTARRS, WISE, and LSST. Finally I ask, now we have opened up essentially allwavelength windows, whether the exploration of survey discovery space is ended.I examine other possible axes of discovery space, and find them mostly to betoo expensive to explore or otherwise unfruitful, with two exceptions : thefirst is the time axis, which we have only just begun to explore properly; andthe second is the possibility of neutrino astrophysics.


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Input: The nonadiabatic Heisenberg model (NHM) proposed as an extension of theHeisenberg model makes a contribution to the eigenstate problem ofsuperconductivity. The Hamiltonian H^n derived within this group-theoreticalmodel has superconducting eigenstates if and only if the considered materialpossesses a narrow, roughly half-filled "superconducting" energy band ofspecial symmetry in its band structure. This paper shows that thehigh-temperature superconductor YBa_2Cu_3O_7 possesses such a superconductingband. This new result together with previous observations about othersuperconductors and non-superconductors corroborates the theoretical evidencewithin the NHM that stable superconducting states are connected withsuperconducting bands. It is proposed that the type of superconductivity, i.e.,whether the material is a conventional low-T_c or a high-T_c superconductor, isdetermined by the energetically lowest boson excitations that carry the crystalspin 1*hbar and are sufficiently stable to transport this crystal spin-angularmomentum through the crystal. This mechanism provides the electron-phononmechanism that enters the BCS theory in conventional superconductors.


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Input: Inclusive dijet and trijet production in deep inelastic $ep$ scattering hasbeen measured for $10<Q^2<100$ GeV$^2$ and low Bjorken $x$, $10^{-4}<x_{\rmBj}<10^{-2}$. The data were taken at the HERA $ep$ collider with centre-of-massenergy $\sqrt{s} = 318 \gev$ using the ZEUS detector and correspond to anintegrated luminosity of $82 {\rm pb}^{-1}$. Jets were identified in thehadronic centre-of-mass (HCM) frame using the $k_{T}$ cluster algorithm in thelongitudinally invariant inclusive mode. Measurements of dijet and trijetdifferential cross sections are presented as functions of $Q^2$, $x_{\rm Bj}$,jet transverse energy, and jet pseudorapidity. As a further examination oflow-$x_{\rm Bj}$ dynamics, multi-differential cross sections as functions ofthe jet correlations in transverse momenta, azimuthal angles, andpseudorapidity are also presented. Calculations at $\mathcal{O}(\alpha_{s}^3)$generally describe the trijet data well and improve the description of thedijet data compared to the calculation at $\mathcal{O}(\alpha_{s}^2)$.


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Input: We study conditions for the deterministic transformation$\ket{\psi}\longrightarrow\ket{\phi}$ of a bipartite entangled state by aseparable operation. If the separable operation is a local operation withclassical communication (LOCC), Nielsen's majorization theorem providesnecessary and sufficient conditions. For the general case we derive a necessarycondition in terms of products of Schmidt coefficients, which is equivalent tothe Nielsen condition when either of the two factor spaces is of dimension 2,but is otherwise weaker. One implication is that no separable operation canreverse a deterministic map produced by another separable operation, if oneexcludes the case where the Schmidt coefficients of $\ket{\psi}$ and are thesame as those of $\ket{\phi}$. The question of sufficient conditions in thegeneral separable case remains open. When the Schmidt coefficients of$\ket{\psi}$ are the same as those of $\ket{\phi}$, we show that the Krausoperators of the separable transformation restricted to the supports of$\ket{\psi}$ on the factor spaces are proportional to unitaries. When thatproportionality holds and the factor spaces have equal dimension, we findconditions for the deterministic transformation of a collection of several fullSchmidt rank pure states $\ket{\psi_j}$ to pure states $\ket{\phi_j}$.


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Input: The dominant background for observations of gamma-rays in the energy regionabove 50 GeV with Imaging Atmospheric Cherenkov telescopes are cosmic-rayevents. The images of most of the cosmic ray showers look significantlydifferent from those of gamma-rays and are therefore easily discriminated.However, a small fraction of events seems to be indistinguishable fromgamma-rays. This constitutes an irreducible background to the observation ofhigh-energy gamma-ray sources, and limits the sensitivity achievable with agiven instrument. Here, a Monte Carlo study of gamma-like cosmic-ray events ispresented. The nature of gamma-like cosmic-ray events, the shower particlesthat are responsible for the gamma-like appearance, and the dependence of theseresults on the choice of the hadronic interaction model are investigated. Mostof the gamma-like cosmic ray events are characterised by the production ofhigh-energy pi0's early in the shower development which dump most of the showerenergy into electromagnetic sub-showers. Also Cherenkov light from single muonscan mimic gamma-rays in close-by pairs of telescopes. Differences of up to 25%in the collection area for gamma-like proton showers between QGSJet/FLUKA andSibyll/FLUKA simulations have been found.


Instruction: what is the prompt that generates the input?

Input: Many organizations aspire to adopt agile processes to take advantage of thenumerous benefits that it offers to an organization. Those benefits include,but are not limited to, quicker return on investment, better software quality,and higher customer satisfaction. To date however, there is no structuredprocess (at least in the public domain) that guides organizations in adoptingagile practices. To address this problem we present the Agile AdoptionFramework. The framework consists of two components: an agile measurementindex, and a 4-Stage process, that together guide and assist the agile adoptionefforts of organizations. More specifically, the agile measurement index isused to identify the agile potential of projects and organizations. The 4-Stageprocess, on the other hand, helps determine (a) whether or not organizationsare ready for agile adoption, and (b) guided by their potential, what set ofagile practices can and should be introduced.


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Input: We consider constraints on the planetesimal population residing in the disksof AU Microscopii, Beta Pictoris and Fomalhaut taking into account theirobserved thicknesses and normal disk opacities. We estimate that bodies ofradius 5, 180 and 70 km are responsible for initiating the collisional cascadeaccounting for the dust production for AU-Mic, Beta-Pic and Fomalhaut's disks,respectively, at break radii from the star where their surface brightnessprofiles change slope. Larger bodies, of radius 1000km and with surface densityof order 0.01 g/cm^2, are required to explain the thickness of these disksassuming that they are heated by gravitational stirring. A comparison betweenthe densities of the two sizes suggests the size distribution in the largestbodies is flatter than that observed in the Kuiper belt. AU Mic's disk requiresthe shallowest size distribution for bodies with radius greater than 10kmsuggesting that the disk contains planetary embryos experiencing a stage ofrunaway growth.


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Input: In spectroscopy, it is conventional to treat pulses much stronger than thelinewidth as delta-functions. In NMR, this assumption leads to the predictionthat pi pulses do not refocus the dipolar coupling. However, NMR spin echomeasurements in dipolar solids defy these conventional expectations when morethan one pi pulse is used. Observed effects include a long tail in the CPMGecho train for short delays between pi pulses, an even-odd asymmetry in theecho amplitudes for long delays, an unusual fingerprint pattern forintermediate delays, and a strong sensitivity to pi-pulse phase. Experimentsthat set limits on possible extrinsic causes for the phenomena are reported. Wefind that the action of the system's internal Hamiltonian during any real pulseis sufficient to cause the effects. Exact numerical calculations, combined withaverage Hamiltonian theory, identify novel terms that are sensitive toparameters such as pulse phase, dipolar coupling, and system size.Visualization of the entire density matrix shows a unique flow of quantumcoherence from non-observable to observable channels when applying repeated pipulses.


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Input: Three-body resonances in the \bar{K}NN system have been studied within aframework of the \bar{K}NN-\pi YN coupled hannel Faddeev equation. By solvingthe three-body equation the energy dependence of the resonant \bar{K}Namplitude is fully taken into account. The S-matrix pole has been investigatedfrom the eigenvalue of the kernel with the analytic continuation of thescattering amplitude on the unphysical Riemann sheet. The \barKN interaction isconstructed from the leading order term of the chiral Lagrangian usingrelativistic kinematics. The \Lambda(1405) resonance is dynamically generatedin this model, where the \bar{K}N interaction parameters are fitted to the dataof scattering length. As a result we find a three-body resonance of the strangedibaryon system with binding energy, B~79 MeV, and width, \Gamma~74 MeV. Theenergy of the three-body resonance is found to be sensitive to the model of theI=0 \barKN interaction.


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Input: Structure entails function and thus a structural description of the brainwill help to understand its function and may provide insights into manyproperties of brain systems, from their robustness and recovery from damage, totheir dynamics and even their evolution. Advances in the analysis of complexnetworks provide useful new approaches to understanding structural andfunctional properties of brain networks. Structural properties of networksrecently described allow their characterization as small-world, random(exponential) and scale-free. They complement the set of other properties thathave been explored in the context of brain connectivity, such as topology,hodology, clustering, and hierarchical organization. Here we apply new networkanalysis methods to cortical inter-areal connectivity networks for the cat andmacaque brains. We compare these corticocortical fibre networks to benchmarkrewired, small-world, scale-free and random networks, using two analysisstrategies, in which we measure the effects of the removal of nodes andconnections on the structural properties of the cortical networks. The brainnetworks' structural decay is in most respects similar to that of scale-freenetworks. The results implicate highly connected hub-nodes and bottleneckconnections as structural basis for some of the conditional robustness of brainsystems. This informs the understanding of the development of brain networks'connectivity.


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Input: Is it possible to link a set of nodes without using preexisting positionalinformation or any kind of long-range attraction of the nodes? Can the processof generating positional information, i.e. the detection of ``unknown'' nodesand the estabishment of chemical gradients, \emph{and} the process of networkformation, i.e. the establishment of links between nodes, occur in parallel, ona comparable time scale, as a process of co-evolution?  The paper discusses a model where the generation of relevant information forestablishing the links between nodes results from the interaction of many\emph{agents}, i.e. subunits of the system that are capable of performing someactivities. Their collective interaction is based on (indirect) communication,which also includes memory effects and the dissemination of information in thesystem. The relevant (``pragmatic'') information that leads to theestablishment of the links then emerges from an evolutionary interplay ofselection and reamplification.


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Input: We investigate the properties and evolution of accretion tori formed afterthe coalescence of two compact objects. At these extreme densities andtemperatures, the accreting torus is cooled mainly by neutrino emissionproduced primarily by electron and positron capture on nucleons (betareactions). We solve for the disc structure and its time evolution byintroducing a detailed treatment of the equation of state which includesphotodisintegration of helium, the condition of beta-equilibrium, and neutrinoopacities. We self-consistently calculate the chemical equilibrium in the gasconsisting of helium, free protons, neutrons and electron-positron pairs andcompute the chemical potentials of the species, as well as the electronfraction throughout the disc. We find that, for sufficiently large accretionrates (> 10 solar masses per second), the inner regions of the disk becomeopaque and develop a viscous and thermal instability. The identification ofthis instability might be relevant for GRB observations.


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Input: We propose that the CP violating phase in the CKM mixing matrix is identicalto the CP phases responsible for the spontaneous CP violation in the Higgspotential. A specific multi-Higgs model with Peccei-Quinn (PQ) symmetry isconstructed to realize this idea. The CP violating phase does not vanish whenall Higgs masses become large. There are flavor changing neutral current (FCNC)interactions mediated by neutral Higgs bosons at the tree level. However,unlike general multi-Higgs models, the FCNC Yukawa couplings are fixed in termsof the quark masses and CKM mixing angles. Implications for meson-anti-mesonmixing, including recent data on $D-\bar D$ mixing, and neutron electric dipolemoment (EDM) are studied. We find that the neutral Higgs boson masses can be atthe order of one hundred GeV. The neutron EDM can be close to the presentexperimental upper bound.


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Input: The differing M_bh-Luminosity relations presented in McLure & Dunlop, Marconi& Hunt and Erwin et al. have been investigated. A number of issues have beenidentified and addressed in each of these studies, including but not limitedto: the removal of a dependency on the Hubble constant; a correction for dustattenuation in the bulges of disc galaxies; the identification of lenticulargalaxies previously treated as elliptical galaxies; and application of the same(Y|X) regression analysis. These adjustments result in relations which nowpredict similar black hole masses. The optimal K-band relation islog(M_bh/M_sun) = -0.37(+/-0.04)[M_K +24] + 8.29(+/-0.08), with a total (notintrinsic) scatter in log M_bh equal to 0.33 dex. This level of scatter issimilar to the value of 0.34 dex from the M_bh-sigma relation of Tremaine etal. and compares favourably with the value of 0.31 dex from the M_bh-n relationof Graham & Driver. Using different photometric data, consistent relations inthe B- and R-band are also provided, although we do note that the small (N=13)R-band sample used by Erwin et al. is found here to have a slope of-0.30(+/-0.06) and a total scatter of 0.31 dex. Performing a symmetricalregression on the larger K-band sample gives a slope of -0.40, implying M_bh ~L^{1.00}. Implications for galaxy-black hole coevolution, in terms of drymergers, are briefly discussed, as are predictions for intermediate mass blackholes. Finally, as previously noted by Tundo et al., a potential bias in thegalaxy sample used to define the M_bh-L relations is shown and a correctiveformula provided.


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Input: We present cosmological hydrodynamical simulations of galaxy clusters aimedat studying the process of metal enrichment of the intra--cluster medium (ICM).These simulations have been performed by implementing a detailed model ofchemical evolution in the Tree-SPH \gd code. This model allows us to follow themetal release from SNII, SNIa and AGB stars, by properly accounting for thelifetimes of stars of different mass, as well as to change the stellar initialmass function (IMF), the lifetime function and the stellar yields. As such, ourimplementation of chemical evolution represents a powerful instrument to followthe cosmic history of metal production. The simulations presented here havebeen performed with the twofold aim of checking numerical effects, as well asthe impact of changing the model of chemical evolution and the efficiency ofstellar feedback.


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Input: We present a catalogue of morphologically classified bright galaxies in thenorth equatorial stripe (230 deg$^2$) derived from the Third Data Release ofthe Sloan Digital Sky Survey (SDSS). Morphological classification is performedby visual inspection of images in the $g$ band. The catalogue contains 2253galaxies complete to a magnitude limit of $r=16$ after Galactic extinctioncorrection, selected from 2658 objects that are judged as extended in thephotometric catalogue in the same magnitude limit. 1866 galaxies in ourcatalogue have spectroscopic information. A brief statistical analysis ispresented for the frequency of morphological types and mean colours in thecatalogue. A visual inspection of the images reveals that the rate ofinteracting galaxies in the local Universe is approximately 1.5% in the$r\le16$ sample. A verification is made for the photometric catalogue generatedby the SDSS, especially as to its bright end completeness.


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Input: The assessment of highly-risky situations at road intersections have beenrecently revealed as an important research topic within the context of theautomotive industry. In this paper we shall introduce a novel approach tocompute risk functions by using a combination of a highly non-linear processingmodel in conjunction with a powerful information encoding procedure.Specifically, the elements of information either static or dynamic that appearin a road intersection scene are encoded by using directed positional acycliclabeled graphs. The risk assessment problem is then reformulated in terms of aninductive learning task carried out by a recursive neural network. Recursiveneural networks are connectionist models capable of solving supervised andnon-supervised learning problems represented by directed ordered acyclicgraphs. The potential of this novel approach is demonstrated through wellpredefined scenarios. The major difference of our approach compared to othersis expressed by the fact of learning the structure of the risk. Furthermore,the combination of a rich information encoding procedure with a generalizedmodel of dynamical recurrent networks permit us, as we shall demonstrate, asophisticated processing of information that we believe as being a first stepfor building future advanced intersection safety systems


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Input: We study the mechanical response generated by local deformations in jammedpackings of rigid disks. Based on discrete element simulations we determine thecritical force of the local perturbation that is needed to break the mechanicalequilibrium and examine the generated displacement field. Displacements decayas a power law of the distance from the perturbation point. The decay exponentand the critical force exhibit nontrivial dependence on the friction: Bothquantities are nonmonotonic and have a sharp maximum at the frictioncoefficient 0.1. We find that the mechanical response properties are closelyrelated to the problem of force-indeterminacy where similar nonmonotonicbehavior was observed previously. We establish direct connection between thecritical force and the ensemble of static force networks.


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Input: During the epoch of reionization, the formation of radiation sources isaccompanied by the growth of a H- photodissociating flux. We estimate theimpact of this flux on the formation of molecular hydrogen and cooling in thefirst galaxies, assuming different types of radiation sources (e.g. Pop II andPop III stars, miniquasars). We find that H- photodissociation reduces theformation of H2 molecules by a factor of ~1+1000k_s*x/(f_esc*delta), where x isthe mean ionized fraction in the IGM, f_esc is the fraction of ionizing photonsthat escape from their progenitor halos, delta is the local gas overdensity andk_s is an order unity constant which depends on the type of radiation source.By the time a significant fraction of the universe becomes ionized, H-photodissociation may significantly reduce the H2 abundance and, with it, theprimordial star formation rate, delaying the progress of reionization.


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Input: We present new predictions for the galaxy three-point correlation function(3PCF) using high-resolution dissipationless cosmological simulations of a flatLCDM Universe which resolve galaxy-size halos and subhalos. We create realisticmock galaxy catalogs by assigning luminosities and colors to dark matter halosand subhalos, and we measure the reduced 3PCF as a function of luminosity andcolor in both real and redshift space. As galaxy luminosity and color arevaried, we find small differences in the amplitude and shape dependence of thereduced 3PCF, at a level qualitatively consistent with recent measurements fromthe SDSS and 2dFGRS. We confirm that discrepancies between previous 3PCFmeasurements can be explained in part by differences in binning choices. Weexplore the degree to which a simple local bias model can fit the simulated3PCF. The agreement between the model predictions and galaxy 3PCF measurementslends further credence to the straightforward association of galaxies with CDMhalos and subhalos.


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Input: This paper aims to provide a practical example on the assessment andpropagation of input uncertainty for option pricing when using tree-basedmethods. Input uncertainty is propagated into output uncertainty, reflectingthat option prices are as unknown as the inputs they are based on. Optionpricing formulas are tools whose validity is conditional not only on how closethe model represents reality, but also on the quality of the inputs they use,and those inputs are usually not observable. We provide three alternativeframeworks to calibrate option pricing tree models, propagating parameteruncertainty into the resulting option prices. We finally compare our methodswith classical calibration-based results assuming that there is no optionsmarket established. These methods can be applied to pricing of instruments forwhich there is not an options market, as well as a methodological tool toaccount for parameter and model uncertainty in theoretical option pricing.


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Input: Context: HCOOH is one of the more common species in interstellar ices withabundances of 1-5% with respect to solid H2O. Aims: This study aims atcharacterizing the HCOOH spectral features in astrophysically relevant icemixtures in order to interpret astronomical data. Methods: The ices are grownunder high vacuum conditions and spectra are recorded in transmission using aFourier transform infrared spectrometer. Pure HCOOH ices deposited at 15 K and145 K are studied, as well as binary and tertiary mixtures containing H2O, CO,CO2 and CH3OH. The mixture concentrations are varied from 50:50% to ~10:90% forHCOOH:H2O. Binary mixtures of HCOOH:X and tertiary mixtures of HCOOH:H2O:X withX = CO, CO2, and CH3OH, are studied for concentrations of ~10:90% and~7:67:26%, respectively. Results: Pure HCOOH ice spectra show broad bands whichsplit around 120 K due to the conversion of a dimer to a chain-structure. Broadsingle component bands are found for mixtures with H2O. Additional spectralcomponents are present in mixtures with CO, CO2 and CH3OH. The resulting peakposition, full width at half maximum and band strength depend strongly on icestructure, temperature, matrix constituents and the HCOOH concentration.Comparison of the solid HCOOH 5.9, 7.2, and 8.1 micron features withastronomical data toward the low mass source HH 46 and high mass source W 33Ashows that spectra of binary mixtures do not reproduce the observed icefeatures. However, our tertiary mixtures especially with CH3OH match theastronomical data very well. Thus interstellar HCOOH is most likely present intertiary or more complex mixtures with H2O, CH3OH and potentially also CO orCO2, providing constraints on its formation.


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Input: Presently clearing electrodes are being considered as a possible cure ofe-cloud driven problems in existing and future colliders. 'Invisible'electrodes, made of a thin highly resistive layer pasted on a dielectric plate,have been proposed as one of design solutions for the e-cloud clearing. For thefirst time such electrodes were successfully used in the electron-positronaccumulator (EPA) of LEP. Similar electrodes had been using for a long time forion clearing purposes in the DAFNE electron ring. Theoretical considerationsand experimental measurements at DAFNE have revealed a substantial contributionof the ion clearing electrodes (ICE) to the machine broad-band impedance givingrise to several harmful effects degrading the collider performance. In thispaper we discuss the impact of the electrodes on DAFNE beam dynamics, show theresults of ICE wake field and impedance calculations and compare them withavailable experimental data. We also describe the procedure of ICE removal fromthe wiggler sections of the electron ring that has resulted in remarkableimprovements in terms of beam dynamics and geometric luminosity.


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Input: Scaling predictions and results from self-consistent field calculations forbottle-brush polymers with a rigid backbone and flexible side chains under goodsolvent conditions are summarized and their validity and applicability isassessed by a comparison with Monte Carlo simulations of a simple latticemodel. It is shown that under typical conditions, as they are also present inexperiments, only a rather weak stretching of the side chains is realized, andthen the scaling predictions based on the extension of the Daoud-Cotton blobpicture are not applicable.  Also two-component bottle brush polymers are considered, where two types(A,B) of side chains are grafted, assuming that monomers of different kindrepel each other. In this case, variable solvent quality is allowed for, suchthat for poor solvent conditions rather dense cylinder-like structures result.Theories predict ``Janus Cylinder''-type phase separation along the backbone inthis case. The Monte Carlo simulations, using the pruned-enriched Rosenbluthmethod (PERM) then are restricted to rather short side chain length.Nevertheless, evidence is obtained that the phase separation between an A-richpart of the cylindrical molecule and a B-rich part can only occur locally. Thecorrelation length of this microphase separation can be controlled by thesolvent quality. This lack of a phase transition is interpreted by an analogywith models for ferromagnets in one space dimension.


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Input: We prove the Kirillov-Reshetikhin (KR) conjecture in the general case : forall twisted quantum affine algebras we prove that the characters of KR modulessolve the twisted Q-system and we get explicit formulas for the character oftheir tensor products (the untwisted simply-laced case was treated by Najakima,and the untwisted case by the author). The proof is uniform and providesseveral new developments for the representation theory of twisted quantumaffine algebras, including twisted Frenkel-Reshetikhin q-characters (expectedby Frenkel-Reshetikhin and Frenkel-Mukhin). We also prove the twisted T-system.As an application we get explicit formulas for the twisted q-characters offundamental representations for all types, including the formulas for typesD_4^{(3)}, E_6^{(2)} conjectured by Reshetikhin. We prove the formulas for KRmodules in types A_n^{(2)} and D_4^{(3)} conjectured by Kuniba-Suzuki.Eventually our results imply the conjectural branching rules [HKOTT] to thequantum subalgebra of finite type.


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Input: The gargantuan discrepancy between the value of the observed cosmologicalconstant and that expected from the zero-point energy of known matter fieldscan be eliminated by supposing that on macroscopic scales the overwhelmingmajority of any volume of spacetime is literal nothingness. This nothingness orvoid results from the proliferative nucleation of tiny void bubbles (a.k.a."bubbles of nothing" or "semi wormholes") that expand until their surfaces,presumed to be 2-branes, collide. This process results in a dense packing ofvoid bubbles of various sizes that leaves only the vanishing interstitialregions between bubbles for spacetime to occupy. This vast reduction in theamount of actual space contained within any apparent volume, reducescorrespondingly the effective zero-point energy density. Unlike previouswormhole-based attempts at vacuum energy suppression, the current approach isentirely Lorentzian and results in a nonzero value for the cosmologicalconstant.


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Input: We present a study of eegamma and mumugamma events using 1109 (1009) pb-1 ofdata in the electron (muon) channel, respectively. These data were collectedwith the D0 detector at the Fermilab Tevatron ppbar Collider at sqrt(s) = 1.96TeV. Having observed 453 (515) candidates in the eegamma (mumugamma) finalstate, we measure the Zgamma production cross section for a photon withtransverse energy ET > 7 GeV, separation between the photon and leptons DeltaR(lgamma) > 0.7, and invariant mass of the di-lepton pair M(ll) > 30 GeV/c^2,to be 4.96 +/- 0.30(stat. + syst.) +/- 0.30(lumi.) pb, in agreement with thestandard model prediction of 4.74 +/- 0.22 pb. This is the most precise Zgammacross section measurement at a hadron collider. We set limits on anomaloustrilinear Zgammagamma and ZZgamma gauge boson couplings of -0.085 <h(30)^(gamma) < 0.084, -0.0053 < h(40)^(gamma) < 0.0054 and -0.083 < h(30)^(Z)< 0.082, -0.0053 < h(40)^(Z) < 0.0054 at the 95% C.L. for the form-factor scaleLambda = 1.2 TeV.


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Input: We present the first systematic investigation of the [NeV] (14um/24um) and[SIII] (18um/33um) infrared line flux ratios, traditionally used to estimatethe density of the ionized gas, in a sample of 41 Type 1 and Type 2 activegalactic nuclei (AGNs) observed with the Infrared Spectrograph on boardSpitzer. The majority of galaxies with both [NeV] lines detected have observed[NeV] line flux ratios consistent with or below the theoretical low densitylimit, based on calculations using currently available collision strengths andignoring absorption and stimulated emission. We find that Type 2 AGNs havelower line flux ratios than Type 1 AGNs and that all of the galaxies with lineflux ratios below the low density limit are Type 2 AGNs. We argue thatdifferential infrared extinction to the [NeV] emitting region due to dust inthe obscuring torus is responsible for the ratios below the low density limitand we suggest that the ratio may be a tracer of the inclination angle of thetorus to our line of sight. Because the temperature of the gas, the amount ofextinction, and the effect of absorption and stimulated emission on the lineratios are all unknown, we are not able to determine the electron densitiesassociated with the [NeV] line flux ratios for the objects in our sample. Wealso find that the [SIII] emission from the galaxies in our sample is extendedand originates primarily in star forming regions. Since the emission fromlow-ionization species is extended, any analysis using line flux ratios fromsuch species obtained from slits of different sizes is invalid for most nearbygalaxies.


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Input: The Large Area Telescope (LAT) instrument onboard GLAST offers a tremendousopportunity for future blazar studies. In order to fully benefit from itscapabilities and to maximize the scientific return from the LAT, it is of greatimportance to conduct dedicated multi-frequency monitoring campaigns that willresult comprehensive observations. Consequently, we initiated an effort toconduct a GLAST-dedicated, quasi-simultaneous, broad-band flux-density (andpolarization) monitoring of potential GLAST blazars with the Effelsberg andOVRO radio telescopes (11cm to 7mm wavelength). Here, we present a shortoverview of these activities which will complement the multi-wavelengthsactivities of the GLAST/LAT collaboration towards the 'low-energy' radio bands.Further we will give a brief outlook including the extension of thiscoordinated campaign towards higher frequencies and future scientific aims.


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Input: Position determination in biological systems is often achieved throughprotein concentration gradients. Measuring the local concentration of such aprotein with a spatially-varying distribution allows the measurement ofposition within the system. In order for these systems to work effectively,position determination must be robust to noise. Here, we calculate fundamentallimits to the precision of position determination by concentration gradientsdue to unavoidable biochemical noise perturbing the gradients. We focus ongradient proteins with first order reaction kinetics. Systems of this type havebeen experimentally characterised in both developmental and cell biologysettings. For a single gradient we show that, through time-averaging, greatprecision can potentially be achieved even with very low protein copy numbers.As a second example, we investigate the ability of a system with oppositelydirected gradients to find its centre. With this mechanism, positionalprecision close to the centre improves more slowly with increasing averagingtime, and so longer averaging times or higher copy numbers are required forhigh precision. For both single and double gradients, we demonstrate theexistence of optimal length scales for the gradients, where precision ismaximized, as well as analyzing how precision depends on the size of theconcentration measuring apparatus. Our results provide fundamental constraintson the positional precision supplied by concentration gradients in variouscontexts, including both in developmental biology and also within a singlecell.


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Input: Very much like the ubiquitous quantum interference of a single particle withitself, quantum interference of two independent, but indistinguishable,particles is also possible. This interference is a direct result of quantumexchange statistics, however, it is observed only in the joint probability tofind the particles in two separated detectors. Here we report the firstobservation of such interference fringes between two independent andnon-interacting electrons in an interferometer proposed by Yurke et al. andSamuelsson et al. Our experiment resembles the "Hanbury Brown and Twiss" (HBT)experiment, which was performed with classical waves. In the experiment, twoindependent and mutually incoherent electron beams were each partitioned intotwo trajectories. The combined four trajectories enclosed an Aharonov-Bohm (AB)flux (but not the two trajectories of a single electron). While individualcurrents were found to be independent of the AB flux, as expected, thecross-correlation between current fluctuations in two opposite points acrossthe device exhibited strong AB oscillations. This is a direct signature oforbital entanglement between two electrons even though they never interact witheach other.


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Input: The extraordinary astrometric accuracy of radio interferometry creates animportant and unique opportunity for the discovery and characterization ofexo-planets. Currently, the Very Long Baseline Array can routinely achievebetter than 100 microarcsecond accuracy, and can approach 10 microarcsecondwith careful calibration. We describe here RIPL, the Radio InterferometricPLanet search, a new program with the VLBA and the Green Bank 100 m telescopethat will survey 29 low-mass, active stars over 3 years with sub-Jovian planetmass sensitivity at 1 AU. An upgrade of the VLBA bandwidth will increaseastrometric accuracy by an order of magnitude. Ultimately, the colossalcollecting area of the Square Kilometer Array could push astrometric accuracyto 1 microarcsecond, making detection and characterizaiton of Earth massplanets possible.  RIPL and other future radio astrometric planet searches occupy a uniquevolume in planet discovery and characterization parameter space. The parameterspace of astrometric searches gives greater sensitivity to planets at largeradii than radial velocity searches. For the VLBA and the expanded VLBA, thetargets of radio astrometric surveys are by necessity nearby, low-mass, activestars, which cannot be studied efficiently through the radial velocity method,coronagraphy, or optical interferometry. For the SKA, detection sensitivitywill extend to solar-type stars. Planets discovered through radio astrometricmethods will be suitable for characterization through extreme adaptive optics.  The complementarity of radio astrometric techniques with other methodsdemonstrates that radio astrometry can play an important role in the roadmapfor exoplanet discovery and characterization.


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Input: We propose a method to study the epoch of reionization based on the possibleobservation of 2p--2s fine structure lines from the neutral hydrogen outsidethe cosmological H {\sc ii} regions enveloping QSOs and other ionizing sourcesin the reionization era. We show that for parameters typical of luminoussources observed at $z \simeq 6.3$ the strength of this signal, which isproportional to the H {\sc i} fraction, has a brightness temperature $\simeq 20  \mu K$ for a fully neutral medium. The fine structure line from this redshiftis observable at $\nu \simeq 1 \rm GHz$ and we discuss prospects for thedetection with several operational and future radio telescopes. We also computethe characteristics of this signal from the epoch of recombination: the peakbrightness is expected to be $\simeq 100 \mu K$; this signal appears in thefrequency range 5-10 MHz. The signal from the recombination era is nearlyimpossible to detect owing to the extreme brightness of the Galactic emissionat these frequencies.


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Input: Following the recent insight in the material structure of comets,protoplanetesimals are assumed to have low densities and to be highly porousagglomerates. It is still unclear if planetesimals can be formed from theseobjects by collisional growth. Therefore, it is important to study numericallythe collisional outcome from low velocity impacts of equal sized porousagglomerates which are too large to be examined in a laboratory experiment. Weuse the Lagrangian particle method Smooth Particle Hydrodynamics to solve theequations that describe the dynamics of elastic and plastic bodies.Additionally, to account for the influence of porosity, we follow a previousdeveloped equation of state and certain relations between the material strengthand the relative density. Collisional growth seems possible for rather lowcollision velocities and particular material strengths. The remnants ofcollisions with impact parameters that are larger than 50% of the radius of thecolliding objects tend to rotate. For small impact parameters, the collidingobjects are effectively slowed down without a prominent compaction of theporous structure, which probably increases the possibility for growth. Theprotoplanetesimals, however, do not stick together for the most part of theemployed material strengths. An important issue in subsequent studies has to bethe influence of rotation to collisional growth. Moreover, for realisticsimulations of protoplanetesimals it is crucial to know the correct materialparameters in more detail.


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Input: Author details research on the new, very prospective, electrostatic SpaceElevator climber based on a new electrostatic linear engine previously offeredat the 42nd Joint Propulsion Conference (AIAA-2006-5229) and published in AEAT,Vol.78, No.6, 2006, pp. 502-508. The electrostatic climber discussed can haveany speed (and braking), the energy for climber movement is delivered by alightweight high-voltage line into a Space Elevator-holding cable from Earthelectric generator. This electric line also can be used for delivery electricenergy to a Geosynchronous Space Station. At present, the best solution of theclimber problem (announced by NASA as one important awarding problem of SpaceElevator) is problematic.  Author also shows the linear electrostatic engine may be used as realisticpower space launcher at the present time. Two projects illustrate these newdevices.  Key words: Space elevator, Electrostatic climber for space elevator,Electrostatic space launcher, Electrostatic accelerator.  This work is presented as paper AIAA-2007-5838 for 43 Joint PropulsionConference, Cincinnati, Ohio, USA, 9-11 July, 2007,


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Input: We search for galaxy counterparts to damped Lyman-alpha absorbers (DLAs) atz>2 towards nine quasars, which have 14 DLAs and 8 sub-DLAs in their spectra.We use integral field spectroscopy to search for Ly-alpha emission line objectsat the redshifts of the absorption systems. Besides recovering two previouslyconfirmed objects, we find six statistically significant candidate Ly-alphaemission line objects. The candidates are identified as having wavelengthsclose to the DLA line where the background quasar emission is absorbed. Incomparison with the six currently known Ly-alpha emitting DLA galaxies thecandidates have similar line fluxes and line widths, while velocity offsetsbetween the emission lines and systemic DLA redshifts are larger. The impactparameters are larger than 10 kpc, and lower column density systems are foundat larger impact parameters. Assuming that a single gas cloud extends from theQSO line of sight to the location of the candidate emission line, we find thatthe average candidate DLA galaxy is surrounded by neutral gas with anexponential scale length of ~5 kpc.


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Input: This paper compares two neural network input selection schemes, the PrincipalComponent Analysis (PCA) and the Automatic Relevance Determination (ARD) basedon Mac-Kay's evidence framework. The PCA takes all the input data and projectsit onto a lower dimension space, thereby reduc-ing the dimension of the inputspace. This input reduction method often results with parameters that havesignificant influence on the dynamics of the data being diluted by those thatdo not influence the dynamics of the data. The ARD selects the most relevantinput parameters and discards those that do not contribute significantly to thedynamics of the data being modelled. The ARD sometimes results with importantinput parameters being discarded thereby compromising the dynamics of the data.The PCA and ARD methods are implemented together with a Multi-Layer-Perceptron(MLP) network for fault identification in structures and the performance of thetwo methods is as-sessed. It is observed that ARD and PCA give similaraccu-racy levels when used as input-selection schemes. There-fore, the choiceof input-selection scheme is dependent on the nature of the data beingprocessed.


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Input: Electronic structure of stripe ordered La$_{2-x}$Sr$_{x}$NiO$_{4}$ isinvestigated. The system with x=1/3 is insulator, in LSDA+U calculations, andshows charge and spin stripe, consistent with the experimental results. Highlycorrelated system of x=1/2 is studied by using exact diagonalization ofmulti-orbital many body Hamiltonian derived from LDA calculations and includingon-site and inter-site Coulomb interactions. The fluctuation of the residualspin on Ni$^{3+}$ (hole) site couples with the charge fluctuation betweenNi$^{3+}$ and Ni$^{2+}$ states and this correlation lowers the total energy.The resultant ground state is insulator with charge and spin stripe of theenergy gap 0.9eV, consistent with observed one. The on-site Coulomb interactionstabilizes integral valency of each Ni ion (Ni$^{3+}$ and Ni$^{2+}$), but doesnot induce the charge order. Two quantities, inter-site Coulomb interaction andanisotropy of hopping integrals, play an important role to form the charge andspin stripe order in a system of x=1/2.


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Input: We determine the masses and decay constants of the pseudoscalar mesons Bs andBc, and also the masses of the vector mesons Bs^* and Bc^*, in quenched latticeQCD with exact chiral symmetry. For 100 gauge configurations generated withsingle-plaquette action at beta = 7.2 on the 32^3 x 60 lattice, we computepoint-to-point quark propagators for 33 quark masses in the range [0.01, 0.85],and measure the time-correlation functions of pseudoscalar and vector mesons.The inverse lattice spacing and the charm quark bare mass are determined usingthe mass and decay constant of eta_c(2980). The bare masses of s and b quarksare chosen such that the masses of the corresponding vector mesons are in goodagreement with phi(1020), and Upsilon(9460) respectively. Our results are:m_{Bs} = 5385(27)(17) MeV, f_{Bs} = 253(8)(7) MeV, m_{Bc} = 6278(6)(4) MeV,f_{Bc} = 489(4)(3) MeV, m_{Bs^*} = 5424(28)(19) MeV, and m_{Bc^*} = 6315(6)(5)MeV.


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Input: We discuss the impact of charged massive particle big bangnucleosynthesis(CBBN) to explore the nature of the reheating of the Universe inthe case that a new extremely long-lived charged massive particle(CHAMP)exists. If the mass of the CHAMP is within collider reach and it's lifetime islonger than $10^4$sec, the comparison between the CBBN prediction and observed$^6$Li abundances may indicate nonstandard reheating in the early Universewithout relying on details of the decay properties. Even if the CHAMP mass isoutside the reach of colliders, the cosmological considerations may provide anontrivial hint for the existence of such very heavy long-lived CHAMPs from thelate Universe if the daughter particles are the dominant component of thepresent dark matter. We consider a low reheating temperature model as anexample of the nonstandard reheating scenarios.


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Input: We consider a stationary and ergodic random field {\omega(b)} parameterizedby the family of bonds b in Z^d, d>1. The random variable \omega(b) is thoughtof as the conductance of bond b and it ranges in a finite interval [0,c_0].Assuming that the set of bonds with positive conductance has a unique infinitecluster C, we prove homogenization results for the random walk among randomconductances on C. As a byproduct, applying the general criterion of \cite{F}leading to the hydrodynamic limit of exclusion processes with bond-dependenttransition rates, for almost all realizations of the environment we prove thehydrodynamic limit of simple exclusion processes among random conductances onC. The hydrodynamic equation is given by a heat equation whose diffusion matrixdoes not depend on the environment. We do not require any ellipticitycondition. As special case, C can be the infinite cluster of supercriticalBernoulli bond percolation.