Instruction: what is the prompt that generates the input?

Input: We consider an electrostatic qubit, interacting with a fluctuating charge ofsingle electron transistor (SET) in the framework of exactly solvable model.The SET plays a role of the fluctuating environment affecting the qubit'sparameters in a controllable way. We derive the rate equations describingdynamics of the entire system for both weak and strong qubit-SET coupling.Solving these equation we obtain decoherence and relaxation rates of the qubit,as well as the spectral density of the fluctuating qubit's parameters. We foundthat in the weak coupling regime the decoherence and relaxation rates aredirectly related to the spectral density taken at Rabi or at zero frequency,depending on what a particular qubit's parameters is fluctuating. This relationholds also in the presence of weak back-action of the qubit on the fluctuatingenvironment. In the case of strong back-action, such simple relationship nolonger holds, even if the qubit-SET coupling is small. It does not hold eitherin the strong-coupling regime, even in the absence of the back-action. Inaddition, we found that our model predicts localization of the qubit in thestrong-coupling regime, resembling that of the spin-boson model.


Instruction: what is the prompt that generates the input?

Input: Studying the internal structure of extragalactic jets is crucial forunderstanding their physics. The Japanese-led space VLBI project VSOP haspresented an opportunity for such studies, by reaching baseline lengths of upto 36,000 km and resolving structures down to an angular size of $\approx 0.3$mas at 5 GHz. VSOP observations of the jet in 0836+710 at 1.6 and 5 GHz haveenabled tracing of the radial structure of the flow on scales from 2 mas to 200mas along the jet and determination of the wavelengths of individualoscillatory modes responsible for the formation of the structure observed. Weapply linear stability analysis to identify the oscillatory modes with modes ofKelvin-Helmholtz instability that match the wavelengths of the structuresobserved. We find that the jet structure in 0836+710 can be reproduced by thehelical surface mode and a combination of the helical and elliptic body modesof Kelvin-Helmholtz instability. Our results indicate that the jet issubstantially stratified and different modes of the instability grow inside thejet at different distances to the jet axis. The helical surface mode can bedriven externally, and we discuss the implications of the driving frequency onthe physics of the active nucleus in 0836+710.


Instruction: what is the prompt that generates the input?

Input: Is it possible to understand cancer? Or more specifically, is it possible tounderstand cancer from genetic side? There already many answers in literature.The most optimistic one has claimed that it is mission-possible. Duesberg andhis colleagues reviewed the impressive amount of research results on canceraccumulated over 100 years. It confirms the a general opinion that consideringall available experimental results and clinical observations there is no cancertheory without major difficulties, including the prevailing gene-based cancertheories. They have then listed 9 "absolute discrepancies" for such cancertheory. In this letter the quantitative evidence against one of their majorreasons for dismissing mutation cancer theory, by both in vivo experiment and afirst principle computation, is explicitly pointed out.


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Input: A combination of the memory function formalism and time-dependentdensity-functional theory is applied to transport in dilute magneticsemiconductors. The approach considers spin and charge disorder andelectron-electron interaction on an equal footing. Within the weak disorderlimit and using a simple parabolic approximation for the valence band we showthat Coulomb and exchange scattering contributions to the resistivity in GaMnAsare of the same order of magnitude. The positional correlations of defectsresult in a significant increase of Coulomb scattering, while the suppressionof localized spin fluctuations in the ferromagnetic phase contributessubstantially to the experimentally observed drop of resistivity below T_c. Aproper treatment of dynamical screening and collective excitations is essentialfor an accurate description of infrared absorption.


Instruction: what is the prompt that generates the input?

Input: The operator-valued Schur-class is defined to be the set of holomorphicfunctions $S$ mapping the unit disk into the space of contraction operatorsbetween two Hilbert spaces. There are a number of alternate characterizations:the operator of multiplication by $S$ defines a contraction operator betweentwo Hardy Hilbert spaces, $S$ satisfies a von Neumann inequality, a certainoperator-valued kernel associated with $S$ is positive-definite, and $S$ can berealized as the transfer function of a dissipative (or even conservative)discrete-time linear input/state/output linear system. Various multivariablegeneralizations of this class have appeared recently,one of the mostencompassing being that of Muhly and Solel where the unit disk is replaced bythe strict unit ball of the elements of a dual correspondence $E^{\sigma}$associated with a $W^{*}$-correspondence $E$ over a $W^{*}$-algebra $\cA$together with a $*$-representation $\sigma$ of $\cA$. The main new point whichwe add here is the introduction of the notion of reproducing kernel Hilbertcorrespondence and identification of the Muhly-Solel Hardy spaces asreproducing kernel Hilbert correspondences associated with a completelypositive analogue of the classical Szeg\"o kernel. In this way we are able tomake the analogy between the Muhly-Solel Schur class and the classical Schurclass more complete. We also illustrate the theory by specializing it to somewell-studied special cases; in some instances there result new kinds ofrealization theorems.


Instruction: what is the prompt that generates the input?

Input: One of the goals of the landscape program in string theory is to extractinformation about the space of string vacua in the form of statisticalcorrelations between phenomenological features that are otherwise uncorrelatedin field theory. Such correlations would thus represent predictions of stringtheory that hold independently of a vacuum-selection principle. In this paper,we study statistical correlations between two features which are likely to becentral to any potential description of nature at high energy scales: gaugesymmetries and spacetime supersymmetry. We analyze correlations between thesetwo kinds of symmetry within the context of perturbative heterotic stringvacua, and find a number of striking features. We find, for example, that thedegree of spacetime supersymmetry is strongly correlated with the probabilitiesof realizing certain gauge groups, with unbroken supersymmetry at the stringscale tending to favor gauge-group factors with larger rank. We also find thatnearly half of the heterotic landscape is non-supersymmetric and yettachyon-free at tree level; indeed, less than a quarter of the tree-levelheterotic landscape exhibits any supersymmetry at all at the string scale.


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Input: A large symmetry group is perhaps experimentally observed in excited hadronswhich includes the chiral group U(2)_L x U(2)_R as a subgroup. To possess thislarge symmetry a dynamical model for excited hadrons, presumably a stringmodel, should explain formation of chiral multiplets and, at the same time,predict coinciding slopes of the angular and radial Regge trajectories. This ispossible only if both the dynamics of the string and the chirality of thequarks at the ends of the string are considered together. We construct amodel-independent unitary transformation from the relativistic chiral basis tothe ^{2S+1}L_J basis, commonly used in hadronic phenomenology as well as in thestring models, and demonstrate that a hadron belonging to the given chiralrepresentation is a fixed superposition of the basis vectors with different L'sand S's. Thus the description of highly excited hadron in terms of a fixed L isnot compatible with chiral symmetry and has to be disregarded in favour of thedescription in terms of the total hadron spin J. Therefore, dynamics of thestring must deliver the principal quantum number ~n+J, in order chiralmultiplets with different spins to become degenerate, as required by the largesymmetry group.


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Input: If dark matter decays to electromagnetically-interacting particles, it caninject energy into the baryonic gas and thus affect the processes ofrecombination and reionization. This leaves an imprint on the cosmic microwavebackground (CMB): the large-scale polarization is enhanced, and the small-scaletemperature fluctuation is damped. We use the WMAP three-year data combinedwith galaxy surveys to constrain radiatively decaying dark matter. Our newlimits to the dark-matter decay width are about ten times stronger thanprevious limits. For dark-matter lifetimes that exceed the age of the Universe,a limit of $\zeta \Gamma_{\chi} < 1.7 \times 10^{-25} s^{-1}$ (95% CL) isderived, where $\zeta$ is the efficiency of converting decay energy intoionization energy. Limits for lifetimes short compared with the age of theUniverse are also derived. We forecast improvements expected from the Plancksatellite.


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Input: Superfluid 3He-A shares the properties of spin nematic and chiral orbitalferromagnet. Its order parameter is characterized by two vectors d and l. Thisdoubly anisotropic superfluid, when it is confined in aerogel, represents themost interesting example of a system with continuous symmetry in the presenceof random anisotropy disorder. We discuss the Larkin-Imry-Ma state, which ischaracterized by the short-range orientational order of the vector l, while thelong-range orientational order is destroyed by the collective action of therandomly oriented aerogel strings. On the other hand, sufficiently largeregular anisotropy produced either by the deformation of the aerogel or byapplied superflow suppresses the Larkin-Imry-Ma effect leading to the uniformorientation of the vector l. This interplay of regular and random anisotropyallows us to study many different effects.


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Input: The ever-increasing knowledge of the structure of various real-world networkshas uncovered their complex multi-mechanism-governed evolution processes.Therefore, a better understanding of the structure and evolution of thesenetworked complex systems requires us to describe such processes in a moredetailed and realistic manner. In this paper, we introduce a new type ofnetwork growth rule which comprises addition and deletion of nodes, and proposean evolving network model to investigate the effect of node deleting on networkstructure. It is found that, with the introduction of node deleting, networkstructure is significantly transformed. In particular, degree distribution ofthe network undergoes a transition from scale-free to exponential forms as theintensity of node deleting increases. At the same time, nontrivialdisassortative degree correlation develops spontaneously as a natural result ofnetwork evolution in the model. We also demonstrate that node deletingintroduced in the model does not destroy the connectedness of a growing networkso long as the increasing rate of edges is not excessively small. In addition,it is found that node deleting will weaken but not eliminate the small-worldeffect of a growing network, and generally it will decrease the clusteringcoefficient in a network.


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Input: The bandstructure was calculated by the full-potential linearized augmentedplane wave method. The result reveals two important insights to the novelsecond harmonic generation (SHG) of alpha-phase lithium iodate($\alpha-LiIO_{3}$) crystal: the existence of finite intra-band momentum matrixelements due to the non-inversion symmetry of the crystal illuminating thepotential of the intra-band transition, and the strong covalent bonding betweenthe $I$-atoms and the ligand $O$-atoms resulting the condition of thedouble-resonance. An inter-band transition scenario in SHG as $\alpha-LiIO_{3}$in nano-structure is proposed. The optical properties were calculated withinthe theoretical framework of the time-dependent perturbation of theindependent-particle model. The dielectric tensors and the refractive indexwere evaluated. Comparisons between the predictions and the results were made:the x-ray near edge absorption spectra; the refractive index at the staticlimit, and at finite frequencies. Possible factors attributing the calculationerrors is discussed.


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Input: This paper analyses the possibilities of performing paralleltransaction-oriented simulations with a special focus on the space-parallelapproach and discrete event simulation synchronisation algorithms that aresuitable for transaction-oriented simulation and the target environment of AdHoc Grids. To demonstrate the findings a Java-based paralleltransaction-oriented simulator for the simulation language GPSS/H isimplemented on the basis of the promising Shock Resistant Time Warpsynchronisation algorithm and using the Grid framework ProActive. Thevalidation of this parallel simulator shows that the Shock Resistant Time Warpalgorithm can successfully reduce the number of rolled back Transaction movesbut it also reveals circumstances in which the Shock Resistant Time Warpalgorithm can be outperformed by the normal Time Warp algorithm. The conclusionof this paper suggests possible improvements to the Shock Resistant Time Warpalgorithm to avoid such problems.


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Input: We investigate an evolutional scenario of the FRW universe with the Casimirenergy scaling like $(-)(1+z)^4$. The Casimir effect is used to explain thevacuum energy differences (its value measured from astrophysics is so smallcompared to value obtained from quantum field theory calculations). Thedynamics of the FRW model is represented in terms of a two-dimensionaldynamical system to show all evolutional paths of this model in the phase spacefor all admissible initial conditions. We find also an exact solution for nonflat evolutional paths of Universe driven by the Casimir effect. The maindifference between the FRW model with the Casimir force and the $\Lambda$CDMmodel is that their generic solutions are a set of evolutional paths with abounce solution and an initial singularity, respectively. The evolutionalscenario are tested by using the SNIa data, FRIIb radiogalaxies, baryonoscillation peak and CMB observation. We compare the power of explanation ofthe model considered and the $\Lambda$CDM model using the Bayesian informationcriterion and Bayesian factor. Our investigation of the information criteria ofmodel selection showed the preference of the $\Lambda$CDM model over the modelconsidered. However the presence of negative like the radiation term can removea tension between the theoretical and observed primordial ${}^4$He and Dabundance.


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Input: Although power laws of the Zipf type have been used by many workers to fitrank distributions in different fields like in economy, geophysics, genetics,soft-matter, networks etc., these fits usually fail at the tails. Somedistributions have been proposed to solve the problem, but unfortunately theydo not fit at the same time both ending tails. We show that many different datain rank laws, like in granular materials, codons, author impact in scientificjournal, etc. are very well fitted by a beta-like function. Then we proposethat such universality is due to the fact that a system made from manysubsystems or choices, imply stretched exponential frequency-rank functionswhich qualitatively and quantitatively can be fitted with the proposedbeta-like function distribution in the limit of many random variables. We provethis by transforming the problem into an algebraic one: finding the rank ofsuccessive products of a given set of numbers.


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Input: The photospheres of stars hosting planets have larger metallicity than starslacking planets. In the present work we study the possibility of an earliermetal enrichment of the photospheres by means of impacting planetesimals duringthe first 20-30Myr. Here we explore this contamination process by simulatingthe interactions of an inward migrating planet with a disc of planetesimalinterior to its orbit. The results show the percentage of planetesimals thatfall on the star. We identified the dependence of the planet's eccentricity($e_p$) and time scale of migration ($\tau$) on the rate of infallingplanetesimals. For very fast migrations ($\tau=10^2$yr and $\tau=10^3$yr) thereis no capture in mean motion resonances, independently of the value of $e_p$.Then, due to the planet's migration the planetesimals suffer close approacheswith the planet and more than 80% of them are ejected from the system. For slowmigrations ($\tau=10^5$yr and $\tau=10^6$yr) the percentage of collisions withthe planet decrease with the increase of the planet's eccentricity. For $e_p=0$and $e_p=0.1$ most of the planetesimals were captured in the 2:1 resonance andmore than 65% of them collided with the star. Whereas migration of a Jupitermass planet to very short pericentric distances requires unrealistic high discmasses, these requirements are much smaller for smaller migrating planets. Oursimulations for a slowly migrating 0.1 $M_{\rm Jupiter}$ planet, even demandinga possible primitive disc three times more massive than a primitive solarnebula, produces maximum [Fe/H] enrichments of the order of 0.18 dex. Thesecalculations open possibilities to explain hot Jupiters exoplanetsmetallicities.


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Input: The lowest-Landau-level anyon model becomes nonperiodic in the statisticsparameter when the finite size of the attached flux tubes is taken intoaccount. The finite-size effects cause the inverse proportional relationbetween the critical filling factor and the statistics parameter to benonperiodically continued in the screening regime, where the fluxes areanti-parallel to the external magnetic field -- at critical filling, theexternal magnetic field is entirely screened by the mean magnetic fieldassociated with the flux tubes. A clustering argument is proposed to selectparticular values of the statistics parameter. In this way, IQHE and FQHEfillings are obtained in terms of gapped nondegenerate LLL-anyonic wavefunctions. Jain's series are reproduced without the need to populate higherLandau levels. New FQHE series are proposed, like, in particular, theparticle-hole complementary series of the Laughlin one. For fast-rotatingBose-Einstein condensates, a corresponding clustering argument yieldsparticular fractional filling series.


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Input: Environmental dielectric screening effects on exciton transition energies insingle-walled carbon nanotubes (SWNTs) have been studied quantitatively in therange of dielectric constants from 1.0 to 37 by immersing SWNTs bridged overtrenches in various organic solvents by means of photoluminescence and theexcitation spectroscopies. With increasing environmental dielectric constant($\epsilon_{\rm env}$), both $E_{11}$ and $E_{22}$ exhibited a redshift byseveral tens meV and a tendency to saturate at a $\epsilon_{\rm env} \sim 5$without an indication of significant ($n$,$m$) dependence. The redshifts can beexplained by dielectric screening of the repulsive electron-electroninteraction. The $\epsilon_{\rm env}$ dependence of $E_{11}$ and $E_{22}$ canbe expressed by a simple empirical equation with a power law in $\epsilon_{\rmenv}$, $E_{\rm ii} = E_{\rm ii}^{\infty} + A\epsilon_{\rm env}^{-\alpha}$. Wealso immersed a sample in sodium-dodecyl-sulfate (SDS) solution to investigatethe effects of wrapping SWNTs with surfactant. The resultant $E_{11}$ and$E_{22}$, which agree well with Weisman's data [Nano Lett. {\bf 3}, 1235(2003)], are close to those of $\epsilon_{\rm env}$ of 2. However, in additionto the shift due to dielectric screening, another shift was observed so thatthe ($2n+m$)-family patterns spread more widely, similar to that of theuniaxial-stress-induced shift.


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Input: Magnetic nanoparticles with Neel surface anisotropy, different internalstructures, surface arrangements and elongation are modelled as many-spinsystems. The results suggest that the energy of many-spin nanoparticles cutfrom cubic lattices can be represented by an effective one-spin potentialcontaining uniaxial and cubic anisotropies. It is shown that the values andsigns of the corresponding constants depend strongly on the particle's surfacearrangement, internal structure and elongation. Particles cut from a simplecubic lattice have the opposite sign of the effective cubic term, as comparedto particles cut from the face-centered cubic lattice. Furthermore, otherremarkable phenomena are observed in nanoparticles with relatively strongsurface effects: (i) In elongated particles surface effects can change the signof the uniaxial anisotropy. (ii) In symmetric particles (spherical andtruncated octahedral) with cubic core anisotropy surface effects can change itssign. We also show that the competition between the core and surfaceanisotropies leads to a new energy that contributes to both the 2nd- and4th-order effective anisotropies.


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Input: By generalizing and extending some of the earlier results derived by Maninand Merkulov, a twistor description is given of four-dimensional N-extended(gauged) self-dual supergravity with and without cosmological constant.Starting from the category of (4|4N)-dimensional complex superconformalsupermanifolds, the categories of (4|2N)-dimensional complex quaternionic,quaternionic Kaehler and hyper-Kaehler right-chiral supermanifolds areintroduced and discussed. We then present a detailed twistor description ofthese types of supermanifolds. In particular, we construct supertwistor spacesassociated with complex quaternionic right-chiral supermanifolds, and explainwhat additional supertwistor data allows for giving those supermanifolds ahyper-Kaehler structure. In this way, we obtain a supersymmetric generalizationof Penrose's nonlinear graviton construction. We furthermore give analternative formulation in terms of a supersymmetric extension of LeBrun'sEinstein bundle. This allows us to include the cases with nonvanishingcosmological constant. We also discuss the bundle of local supertwistors andaddress certain implications thereof. Finally, we comment on a real version ofthe theory related to Euclidean signature.


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Input: In spite of the large number of papers appeared in the past which are devotedto the lattice Boltzmann (LB) methods, basic aspects of the theory still remainunchallenged. An unsolved theoretical issue is related to the construction of adiscrete kinetic theory which yields \textit{exactly} the fluid equations,i.e., is non-asymptotic (here denoted as \textit{LB inverse kinetic theory}).The purpose of this paper is theoretical and aims at developing an inversekinetic approach of this type. In principle infinite solutions exist to thisproblem but the freedom can be exploited in order to meet importantrequirements. In particular, the discrete kinetic theory can be defined so thatit yields exactly the fluid equation also for arbitrary non-equilibrium (butsuitably smooth) kinetic distribution functions and arbitrarily close to theboundary of the fluid domain. Unlike previous entropic LB methods the theoremcan be obtained without functional constraints on the class of the initialdistribution functions. Possible realizations of the theory and asymptoticapproximations are provided which permit to determine the fluid equations\textit{with prescribed accuracy.} As a result, asymptotic accuracy estimatesof customary LB approaches and comparisons with the Chorin artificialcompressibility method are discussed.


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Input: 5972 independent and cumulative yields of radioactive residuals nuclei havebeen measured in 55 thin 206,207,208,nat-Pb and 209-Bi targets irradiated by0.04, 0.07, 0.10, 0.15, 0.25, 0.6, 0.8, 1.2, 1.4, 1.6, and 2.6 GeV protons.Besides, 219 yields have been measured in 0.3, 0.5, 0.75, 1.0, 1.5, and 2.6 GeVproton-irradiated 56-Fe target. The protons were extracted from the ITEP U-10synchrotron. The measured data are compared with experimental results obtainedelsewhere and with theoretical calculations by LAHET, MCNPX, CEM03, LAQGSM03,CASCADE, CASCADO, and LAHETO codes. The predictive power was found to bedifferent for each of the codes tested, but was satisfactory on the whole inthe case of spallation products. At the same time, none of the codes cande-scribe well the product yields throughout the whole product mass range, andall codes must be further improved.


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Input: We investigate the hydrodynamics of accretion channelled by a dipolarmagnetic field (funnel flows). We consider situations in which the electronsand ions in the flow cannot maintain thermal equilibrium (two-temperatureeffects) due to strong radiative loss, and determine the effects on the keVX-ray properties of the systems. We apply this model to investigate theaccretion shocks of white dwarfs in magnetic cataclysmic variables. We havefound that the incorporation of two-temperature effects could harden the keVX-rays. Also, the dipolar model yields harder X-ray spectra than the standardplanar model if white dwarf is sufficiently massive (>~1M_sun). When fittingobserved keV X-ray spectra of magnetic cataclysmic variables, the inclusion oftwo-temperature hydrodynamics and a dipolar accretion geometry lowers estimatesfor white-dwarf masses when compared with masses inferred from models excludingthese effects. We find mass reductions <~9% in the most massive cases.


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Input: In this paper we study random induced subgraphs of the binary $n$-cube,$Q_2^n$. This random graph is obtained by selecting each $Q_2^n$-vertex withindependent probability $\lambda_n$. Using a novel construction ofsubcomponents we study the largest component for$\lambda_n=\frac{1+\chi_n}{n}$, where $\epsilon\ge \chi_n\ge n^{-{1/3}+\delta}$, $\delta>0$. We prove that there exists a.s. a unique largestcomponent $C_n^{(1)}$. We furthermore show that $\chi_n=\epsilon$, $|C_n^{(1)}|\sim \alpha(\epsilon) \frac{1+\chi_n}{n} 2^n$ and for $o(1)=\chi_n\gen^{-{1/3}+\delta}$, $| C_n^{(1)}| \sim 2 \chi_n \frac{1+\chi_n}{n} 2^n$ holds.This improves the result of \cite{Bollobas:91} where constant $\chi_n=\chi$ isconsidered. In particular, in case of $\lambda_n=\frac{1+\epsilon} {n}$, ouranalysis implies that a.s. a unique giant component exists.


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Input: We discuss Kondo behavior of a conduction electron system coupled with localoptical phonon by analyzing the Anderson-Holstein model with the use of anumerical renormalization group (NRG) method. There appear three typicalregions due to the balance between Coulomb interaction $U_{\rm ee}$ andphonon-mediated attraction $U_{\rm ph}$. For $U_{\rm ee}>U_{\rm ph}$, weobserve the standard Kondo effect concerning spin degree of freedom. Since theCoulomb interaction is effectively reduced as $U_{\rm ee}-U_{\rm ph}$, theKondo temperature $T_{\rm K}$ is increased when $U_{\rm ph}$ is increased. Onthe other hand, for $U_{\rm ee}<U_{\rm ph}$, there occurs the Kondo effectconcerning charge degree of freedom, since vacant and double occupied statesplay roles of pseudo-spins. Note that in this case, $T_{\rm K}$ is decreasedwith the increase of $U_{\rm ph}$. Namely, $T_{\rm K}$ should be maximized for$U_{\rm ee} \approx U_{\rm ph}$. Then, we analyze in detail the Kondo behaviorat $U_{\rm ee}=U_{\rm ph}$, which is found to be explained by the polaronAnderson model with reduced hybridization of polaron and residual repulsiveinteraction among polarons. By comparing the NRG results of the polaronAnderson model with those of the original Anderson-Holstein model, we clarifythe Kondo behavior in the competing region of $U_{\rm ee} \approx U_{\rm ph}$.


Instruction: what is the prompt that generates the input?

Input: In object-oriented or object-relational databases such as multimediadatabases or most XML databases, access patterns are not static, i.e.,applications do not always access the same objects in the same orderrepeatedly. However, this has been the way these databases and associatedoptimisation techniques such as clustering have been evaluated up to now. Thispaper opens up research regarding this issue by proposing a dynamic objectevaluation framework (DOEF). DOEF accomplishes access pattern change bydefining configurable styles of change. It is a preliminary prototype that hasbeen designed to be open and fully extensible. Though originally designed forthe object-oriented model, it can also be used within the object-relationalmodel with few adaptations. Furthermore, new access pattern change models canbe added too. To illustrate the capabilities of DOEF, we conducted twodifferent sets of experiments. In the first set of experiments, we used DOEF tocompare the performances of four state of the art dynamic clusteringalgorithms. The results show that DOEF is effective at determining theadaptability of each dynamic clustering algorithm to changes in access pattern.They also led us to conclude that dynamic clustering algorithms can cope withmoderate levels of access pattern change, but that performance rapidly degradesto be worse than no clustering when vigorous styles of access pattern changeare applied. In the second set of experiments, we used DOEF to compare theperformance of two different object stores: Platypus and SHORE. The use of DOEFexposed the poor swapping performance of Platypus.


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Input: Multifrequency VLBA observations of the final group of ten objects in asample of FIRST-based compact steep spectrum (CSS) sources are presented. Thesample was selected to investigate whether objects of this kind could be relicsof radio-loud AGNs switched off at very early stages of their evolution orpossibly to indicate intermittent activity. Initial observations were madeusing MERLIN at 5 GHz. The sources have now been observed with the VLBA at 1.7,5 and 8.4 GHz in a snapshot mode with phase-referencing. The resulting maps arepresented along with unpublished 8.4-GHz VLA images of five sources. Some ofthe sources discussed here show a complex radio morphology and therefore acomplicated past that, in some cases, might indicate intermittent activity. Oneof the sources studied - 1045+352 - is known as a powerful radio andinfrared-luminous broad absorption line (BAL) quasar. It is a young CSS objectwhose asymmetric two-sided morphology on a scale of several hundred parsecs,extending in two different directions, may suggest intermittent activity. Theyoung age and compact structure of 1045+352 is consistent with the evolutionscenario of BAL quasars. It has also been confirmed that the submillimetre fluxof 1045+352 can be seriously contaminated by synchrotron emission.


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Input: Database search has wide applications and is used as a subroutine in manyimportant algorithms. We shall consider a database with one target item.Quantum algorithm finds the target item in a database faster than any classicalalgorithm. It frequently occurs in practice that only a portion of informationabout the target item is interesting, or we need to find a group of itemssharing some common feature as the target item. This problem is in generalformulated as search for a part of the database [a block] containing the targetitem, instead of the item itself. This is partial search. Partial search tradesaccuracy for speed, i.e. it works faster than a full search. Partial searchalgorithm was discovered by Grover and Radhakrishnan. We shall consideroptimized version of the algorithm and call it GRK. It can be appliedsuccessively [in a sequence]. First the database is partitioned into blocks andwe use GRK to find the target block. Then this target block is partitioned intosub-blocks and we use GRK again to find the target sub-block. [We can call itbinary quantum search.] Another possibility is to partition the database intosub-blocks directly and use GRK to find the target sub-block in one time. Inthis paper we prove that the latter is faster [makes less queries to theoracle].


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Input: We compare the CO 2-1 observations against previously taken CO 4-3observations and analyze the spatial distribution of young stellar objects(YSO's) within the cloud using the Spitzer IRAC observations of the 30 Doraduscomplex. Both peaks of CO 2-1 and 4-3 emitting clouds coincide with the densestregion of the filaments where multiple shells are colliding. We find that theYSO's are clustered in the southern ridge of the warm and dense molecular gasclouds traced by CO J=4-3, indicating a filamentary structure of star formationthroughout the 30 Doradus. We also find that some of Class I YSO's candidateswhich are likely to be associated with a high-velocity component of CO 4-3emitting clouds are present. This is a bona fide place where the triggered starformation had happened and newly formed stars may have produced such ahigh-velocity outflow interacting with the surrounding molecular cloudmaterial.


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Input: We present ACS/HST coronagraphic observations of HD 100546, a B9.5 star, 103pc away from the sun, taken in the F435W, F606W, and F814W bands. Scatteredlight is detected up to 14'' from the star. The observations are consistentwith the presence of an extended flattened nebula with the same inclination asthe inner disk. The well-known ``spiral arms'' are clearly observed and theytrail the rotating disk material. Weaker arms never before reported are alsoseen. The inter-arm space becomes brighter, but the structures become moreneutral in color at longer wavelengths, which is not consistent with modelsthat assume that they are due to the effects of a warped disk. Along the majordisk axis, the colors of the scattered-light relative to the star are \Delta(F435W-F606W) ~ 0.0--0.2 mags and \Delta (F435W-F814W)~0.5--1 mags. To explainthese colors, we explore the role of asymmetric scattering, reddening, andlarge minimum sizes on ISM-like grains. We conclude each of these hypotheses byitself cannot explain the colors. The disk colors are similar to those derivedfor Kuiper Belt objects, suggesting that the same processes responsible fortheir colors may be at work here. We argue that we are observing only thegeometrically thick, optically thin envelope of the disk, while the opticallythick disk responsible for the far-IR emission is undetected. The observedspiral arms are then structures on this envelope. The colors indicate that theextended nebulosity is not a remnant of the infalling envelope but reprocesseddisk material.


Instruction: what is the prompt that generates the input?

Input: We conducted a preliminary field study to understand the current state ofpersonal digital archiving in practice. Our aim is to design a service for thelong-term storage, preservation, and access of digital belongings by examininghow personal archiving needs intersect with existing and emerging archivingtechnologies, best practices, and policies. Our findings not only confirmedthat experienced home computer users are creating, receiving, and finding anincreasing number of digital belongings, but also that they have already lostirreplaceable digital artifacts such as photos, creative efforts, and records.Although participants reported strategies such as backup and file replicationfor digital safekeeping, they were seldom able to implement them consistently.Four central archiving themes emerged from the data: (1) people find itdifficult to evaluate the worth of accumulated materials; (2) personal storageis highly distributed both on- and offline; (3) people are experiencingmagnified curatorial problems associated with managing files in the aggregate,creating appropriate metadata, and migrating materials to maintainable formats;and (4) facilities for long-term access are not supported by the currentdesktop metaphor. Four environmental factors further complicate archiving inconsumer settings: the pervasive influence of malware; consumer reliance on adhoc IT providers; an accretion of minor system and registry inconsistencies;and strong consumer beliefs about the incorruptibility of digital forms, thereliability of digital technologies, and the social vulnerability of networkedstorage.


Instruction: what is the prompt that generates the input?

Input: We investigate the mass function in the substellar domain down to a fewJupiter masses in the young sigma Orionis open cluster (3+/-2 Ma, d =360^+70_-60 pc). We have performed a deep IJ-band search, covering an area of790 arcmin^2 close to the cluster centre. This survey was complemented with aninfrared follow-up in the HKs- and Spitzer 3.6-8.0 mum-bands. Usingcolour-magnitude diagrams, we have selected 49 candidate cluster members in themagnitude interval 16.1 mag < I < 23.0 mag. Accounting for flux excesses at 8.0mum and previously known spectral features of youth, 30 objects are bona fidecluster members. Four are first identified from our optical-near infrared data.Eleven have most probable masses below the deuterium burning limit and areclassified as planetary-mass object candidates. The slope of the substellarmass spectrum (Delta N / Delta M = a M^-alpha) in the mass interval 0.11 Msol M< 0.006 Msol is alpha = +0.6+/-0.2. Any opacity mass-limit, if these objectsform via fragmentation, may lie below 0.006 Msol. The frequency of sigmaOrionis brown dwarfs with circumsubstellar discs is 47+/-15 %. The continuityin the mass function and in the frequency of discs suggests that very low-massstars and substellar objects, even below the deuterium-burning mass limit, mayshare the same formation mechanism.


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Input: We consider that the pre-inflation era is radiation-dominated, transitingsmoothly to the inflationary era. We work out in detail the dynamics ofinflaton fluctuations across the phase transition and the proper choices ofinitial vacuum states. It is found that this phase transition can suppresslong-wavelength quantum fluctuations of inflaton. This may attribute to thelarge-scale CMB anisotropy a lower power than predicted in the standard$\Lambda$CDM model. In constraining this transitional effect by WMAP anisotropydata, we use the WMAP best-fit scale-invariant $\Lambda$CDM model with thedensity power spectrum replaced by the one found in this work. We find that thetransition occurs at least about 10 e-folds before the comoving scalescomparable to our present horizon size cross the Hubble radius duringinflation.


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Input: This paper extends and builds upon the results of an earlier paper, in whichwe described how to use the tools of geometrical engineering to deformgeometrically-engineered grand unified models into ones with lower symmetry.This top-down unfolding has the advantage that the relative positions ofsingularities giving rise to the many `low energy' matter fields are related byonly a few parameters which deform the geometry of the unified model. Andbecause the relative positions of singularities are necessary to compute thesuperpotential, for example, this is a framework in which the arbitrariness ofgeometrically engineered models can be greatly reduced.  In our earlier paper, this picture was made concrete for the case ofdeforming the representations of an SU(5) model into their Standard Modelcontent. In this paper we continue that discussion to show how a geometricallyengineered 16 of SO(10) can be unfolded into the Standard Model, and how thethree families of the Standard Model uniquely emerge from the unfolding of asingle, isolated E8 singularity.


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Input: [Abridged] We have been exploring a spectroscopic unification for all knowntypes of broad line emitting AGN. The 4D Eigenvector 1 (4DE1) parameter spaceshows promise as a unification capable of organizing quasar diversity on asequence primarily governed by Eddington ratio. This paper considers the roleof CIV 1549 measures with special emphasis on the CIV 1549 line shift as aprincipal 4DE1 diagnostic. We use HST archival spectra for 130 sources with S/Nhigh enough to permit reliable CIV 1549 broad component (BC) measures. We finda CIV 1549 BC profile blueshift that is strongly concentrated among (largelyradio-quiet: RQ) sources with FWHM(H beta BC) < 4000 km/s (which we callPopulation A). Narrow line Seyfert 1 (NLSy1, with FWHM H beta < 2000 km/s)sources belong to this population but do not emerge as a distinct class. Thesystematic blueshift, widely interpreted as arising in a disk wind/outflow, isnot observed in broader lined AGN which we call Population B. We find newcorrelations between FWHM(CIV 1549 BC) and CIV 1549 line shift as well as theequivalent width of CIV 1549. They are seen only in Pop. A sources. CIV 1549measures enhance the apparent dichotomy at FWHM(Hbeta BC) approx. 4000 \kms\(Sulentic et al. 2000) suggesting that it has more significance in the contextof Broad Line Region structure than the more commonly discussed RL vs. RQdichotomy. Black hole masses computed from FWHM CIV 1549 BC for about 80 AGNindicate that the CIV 1549 width is a poor virial estimator. Comparison of massestimates derived from Hbeta BC and CIV 1549 reveals that the latter showdifferent and nonlinear offsets for population A and B sources. A significantnumber of sources also show narrow line CIV 1549 emission. We present a recipefor CIV 1549 narrow component extraction.


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Input: In the radio regime the mass-loss rate of AGB stars is best probed usingmolecular (and atomic) line emission arising in the CSE formed by the stellarwind. The numerical modelling of the circumstellar emission where intricateinterplays between physical and chemical processes take place, is a challenge.The derived mass-loss rates depend crucially on the assumptions in thecircumstellar model, of which some can be constrained if enough observationaldata exist. Therefore, a reliable mass-loss-rate determination for anindividual star requires, in addition to a detailed radiative transferanalysis, good observational constraints in the form of multi-line observationsand radial brightness distributions. Of the methods used to estimate mass-lossrates from galactic AGB stars those based on radiative transfer modelling of COline emission are most commonly used and possibly also the most accurate.Typically, CO multi-transitional observations can constrain the mass-loss rateto better than 50%, within the adopted circumstellar model. Comparison withcomplementary methods, such as estimates based on dust radiative transfermodelling coupled with a dynamical model, are consistent within a factor ofthree.


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Input: AU Pegasi is a pulsating star in a spectroscopic binary system with anorbital period of 53.26 days. Between 1960 and 1990 an extremely rapid periodincrease was observed in the value of the pulsation period, but in the last 15years the observation show that the period set in 2.411 days. Fourier analysisof photometric data obtained during the ASAS project and those taken at thePiszkesteto Mountain Station of the Konkoly Observatory during 1994-2005indicate that AU Pegasi is pulsating in two modes simultaneously, and the ratioof the frequencies of the two modes is 0.706, a value common for double-modeclassical Cepheids. A careful analysis of other photometric observationsobtained during the era of the strong period increase also revealed existenceof a second mode. This may suggest that this star is not a Type II Cepheid,despite its galactic position.


Instruction: what is the prompt that generates the input?

Input: We prove that every complete connected immersed surface with positiveextrinsic curvature $K$ in $H^2\times R$ must be properly embedded,homeomorphic to a sphere or a plane and, in the latter case, study the behaviorof the end. Then, we focus our attention on surfaces with positive constantextrinsic curvature ($K-$surfaces). We establish that the only complete$K-$surfaces in $S^2\times R$ and $H^2\times R$ are rotational spheres. Hereare the key steps to achieve this. First height estimates for compact$K-$surfaces in a general ambient space $M^2\times R$ with boundary in a sliceare obtained. Then distance estimates for compact $K-$surfaces (andH-$surfaces) in $H^2\times R$ with boundary on a vertical plane are obtained.Finally we construct a quadratic form with isolated zeroes of negative index.


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Input: We apply a recently developed perturbative formalism which describes theevolution under their self-gravity of particles displaced from a perfectlattice to quantify precisely, up to shell crossing, the effects ofdiscreteness in dissipationless cosmological N-body simulations. We give simpleexpressions, explicitly dependent on the particle density, for the evolution ofpower in each mode as a function of red-shift. For typical starting red-shiftsthe effect of finite particle number is to {\it slow down} slightly the growthof power compared to that in the fluid limit (e.g. by about ten percent at halfthe Nyquist frequency), and to induce also dispersion in the growth as afunction of direction at a comparable level. In the limit that the initialred-shift tends to infinity, at fixed particle density, the evolution in factdiverges from that in the fluid limit (described by the Zeldovichapproximation). Contrary to widely held belief, this means that a simulationstarted at a red-shift much higher than the red-shift of shell crossingactually gives a worse, rather than a better, result. We also study how theseeffects are modified when there is a small-scale regularization of thegravitational force. We show that such a smoothing may reduce the anisotropy ofthe discreteness effects, but it then {\it increases} their average effect.This behaviour illustrates the fact that the discreteness effects describedhere are distinct from those usually considered in this context, due totwo-body collisions. Indeed the characteristic time for divergence from thecollisionless limit is proportional to $N^{2/3}$, rather than $N/ \log N$ inthe latter case.


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Input: We report quantitative relations between corruption level and economicfactors, such as country wealth and foreign investment per capita, which arecharacterized by a power law spanning multiple scales of wealth and investmentsper capita. These relations hold for diverse countries, and also remain stableover different time periods. We also observe a negative correlation betweenlevel of corruption and long-term economic growth. We find similar results fortwo independent indices of corruption, suggesting that the relation betweencorruption and wealth does not depend on the specific measure of corruption.The functional relations we report have implications when assessing therelative level of corruption for two countries with comparable wealth, and forquantifying the impact of corruption on economic growth and foreigninvestments.


Instruction: what is the prompt that generates the input?

Input: We study the properties of the Heisenberg antiferromagnet with spatiallyanisotropic nearest-neighbour exchange couplings on the kagome net, i.e. withcoupling J in one lattice direction and couplings J' along the other twodirections. For J/J' > 1, this model is believed to describe the magneticproperties of the mineral volborthite. In the classical limit, it exhibits twokinds of ground states: a ferrimagnetic state for J/J' < 1/2 and a largemanifold of canted spin states for J/J' > 1/2. To include quantum effectsself-consistently, we investigate the Sp(N) symmetric generalisation of theoriginal SU(2) symmetric model in the large-N limit. In addition to thedependence on the anisotropy, the Sp(N) symmetric model depends on a parameterkappa that measures the importance of quantum effects. Our numericalcalculations reveal that in the kappa-J/J' plane, the system shows a rich phasediagram containing a ferrimagnetic phase, an incommensurate phase, and adecoupled chain phase, the latter two with short- and long-range order. Wecorroborate these results by showing that the boundaries between the variousphases and several other features of the Sp(N) phase diagram can be determinedby analytical calculations. Finally, the application of a block-spinperturbation expansion to the trimerised version of the original spin-1/2 modelleads us to suggest that in the limit of strong anisotropy, J/J' >> 1, theground state of the original model is a collinearly ordered antiferromagnet,which is separated from the incommensurate state by a quantum phase transition.


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Input: We propose a model based on SU(5) x {}^{(d)}T which successfully gives riseto near tri-bimaximal leptonic mixing as well as realistic CKM matrix elementsfor the quarks. The Georgi-Jarlskog relations for three generations are alsoobtained. Due to the {}^{(d)}T transformation property of the matter fields,the b-quark mass can be generated only when the {}^{(d)}T symmetry is broken,giving a dynamical origin for the hierarchy between m_{b} and m_{t}. There areonly nine operators allowed in the Yukawa sector up to at least mass dimensionseven due to an additional Z_{12} x Z'_{12} symmetry, which also forbids, up tosome high orders, operators that lead to proton decay. The resulting model hasa total of nine parameters in the charged fermion and neutrino sectors, andhence is very predictive. In addition to the prediction for \theta_{13} \simeq\theta_{c}/3 \sqrt{2}, the model gives rise to a sum rule,\tan^{2}\theta_{\odot} \simeq \tan^{2} \theta_{\odot, \mathrm{TBM}} - {1/2}\theta_{c} \cos\beta, which is a consequence of the Georgi-Jarlskog relationsin the quark sector. This deviation could account for the difference betweenthe experimental best fit value for the solar mixing angle and the valuepredicted by the tri-bimaximal mixing matrix.


Instruction: what is the prompt that generates the input?

Input: We model the interaction between the wind from a newly formed rapidlyrotating magnetar and the surrounding supernova shock and host star. Thedynamics is modeled using the two-dimensional, axisymmetric thin-shellequations. In the first ~10-100 seconds after core collapse the magnetarinflates a bubble of plasma and magnetic fields behind the supernova shock. Thebubble expands asymmetrically because of the pinching effect of the toroidalmagnetic field, just as in the analogous problem of the evolution of pulsarwind nebulae. The degree of asymmetry depends on E_mag/E_tot. The correct valueof E_mag/E_tot is uncertain because of uncertainties in the conversion ofmagnetic energy into kinetic energy at large radii in relativistic winds; weargue, however, that bubbles inflated by newly formed magnetars are likely tobe significantly more magnetized than their pulsar counterparts. We show thatfor a ratio of magnetic to total power supplied by the central magnetarL_mag/L_tot ~ 0.1 the bubble expands relatively spherically. For L_mag/L_tot ~0.3, however, most of the pressure in the bubble is exerted close to therotation axis, driving a collimated outflow out through the host star. This canaccount for the collimation inferred from observations of long-durationgamma-ray bursts (GRBs). Outflows from magnetars become increasinglymagnetically dominated at late times, due to the decrease in neutrino-drivenmass loss as the young neutron star cools. We thus suggest that themagnetar-driven bubble initially expands relatively spherically, enhancing theenergy of the associated supernova, while at late times it becomesprogressively more collimated, producing the GRB.


Instruction: what is the prompt that generates the input?

Input: We analyse and compare the complexity of several algorithms for computingmodular polynomials. We show that an algorithm relying on floating pointevaluation of modular functions and on interpolation, which has received littleattention in the literature, has a complexity that is essentially (up tologarithmic factors) linear in the size of the computed polynomials. Inparticular, it obtains the classical modular polynomials $\Phi_\ell$ of primelevel $\ell$ in time O (\ell^3 \log^4 \ell \log \log \ell). Besides treatingmodular polynomials for $\Gamma^0 (\ell)$, which are an important ingredient inmany algorithms dealing with isogenies of elliptic curves, the algorithm iseasily adapted to more general situations. Composite levels are handled just aseasily as prime levels, as well as polynomials between a modular function andits transform of prime level, such as the Schl\"afli polynomials and theirgeneralisations. Our distributed implementation of the algorithm confirms thetheoretical analysis by computing modular equations of record level around10000 in less than two weeks on ten processors.


Instruction: what is the prompt that generates the input?

Input: We considered diffusion-driven processes on small-world networks withdistance-dependent random links. The study of diffusion on such networks ismotivated by transport on randomly folded polymer chains, synchronizationproblems in task-completion networks, and gradient driven transport onnetworks. Changing the parameters of the distance-dependence, we found a richphase diagram, with different transient and recurrent phases in the context ofrandom walks on networks. We performed the calculations in two limiting cases:in the annealed case, where the rearrangement of the random links is fast, andin the quenched case, where the link rearrangement is slow compared to themotion of the random walker or the surface. It has been well-established thatin a large class of interacting systems, adding an arbitrarily small densityof, possibly long-range, quenched random links to a regular lattice interactiontopology, will give rise to mean-field (or annealed) like behavior. In somecases, however, mean-field scaling breaks down, such as in diffusion or in theEdwards-Wilkinson process in "low-dimensional" small-world networks. Thisbreak-down can be understood by treating the random links perturbatively, wherethe mean-field (or annealed) prediction appears as the lowest-order term of anaive perturbation expansion. The asymptotic analytic results are alsoconfirmed numerically by employing exact numerical diagonalization of thenetwork Laplacian. Further, we construct a finite-size scaling framework forthe relevant observables, capturing the cross-over behaviors in finitenetworks. This work provides a detailed account of theself-consistent-perturbative and renormalization approaches briefly introducedin two earlier short reports.


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Input: The paper considers pseudo-differential boundary value control systems. Theunderlying operators form an algebra D with the help of which we are able toformulate typical boundary value control problems. The symbolic calculus givestools to form e.g. compositions, formal adjoints, generalized right or leftinverses and compatibility conditions. By a parametrizability we mean that fora given control system Au=0 one finds an operator S such that Au=0 if and onlyif u=Sf. The computation rules of D (or its appropriate subalgebra D')guarantee that in many applications S can be refinely analyzed or evenexplicitly calculated. We outline some methods of homological algebra for thestudy of parametrization S. Especially the projectivity of a certain factormodule (defined by the system equations) implies the parametrizability. We givesome examples to illustrate our computational methods.


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Input: This work reports a theoretical study of the gas phase unimoleculardecomposition of cyclobutane, cyclopentane and cyclohexane by means of quantumchemical calculations. A biradical mechanism has been envisaged for eachcycloalkane, and the main routes for the decomposition of the biradicals formedhave been investigated at the CBS-QB3 level of theory. Thermochemical data(\delta H^0_f, S^0, C^0_p) for all the involved species have been obtained bymeans of isodesmic reactions. The contribution of hindered rotors has also beenincluded. Activation barriers of each reaction have been analyzed to assess the1 energetically most favorable pathways for the decomposition of biradicals.Rate constants have been derived for all elementary reactions using transitionstate theory at 1 atm and temperatures ranging from 600 to 2000 K. Global rateconstant for the decomposition of the cyclic alkanes in molecular products havebeen calculated. Comparison between calculated and experimental results allowedto validate the theoretical approach. An important result is that therotational barriers between the conformers, which are usually neglected, are ofimportance in decomposition rate of the largest biradicals. Ring strainenergies (RSE) in transition states for ring opening have been estimated andshow that the main part of RSE contained in the cyclic reactants is removedupon the activation process.


Instruction: what is the prompt that generates the input?

Input: The Special Theory of Relativity and the Theory of the Electron have had aninteresting history together. Originally the electron was studied in a nonrelativistic context and this opened up the interesting possibility that leadto the conclusion that the mass of the electron could be thought of entirely inelectromagnetic terms without introducing inertial considerations. However theapplication of Special Relativity lead to several problems, both for anextended electron and the point electron. These inconsistencies have, contraryto popular belief not been resolved satisfactorily today, even within thecontext of Quantum Theory. Nevertheless these and subsequent studies bring outthe interesting result that Special Relativity breaks down within the Comptonscale or when the Compton scale is not neglected. This again runs contrary toan uncritical notion that Special Relativity is valid for point particles.


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Input: We have conducted a high-resolution ``3D'' imaging survey of the CO(1--0),HCN(1--0), and HCO$^+$(1--0) lines toward the central a few kpc regions of theSeyfert and starburst galaxies in the local universe using the NobeyamaMillimeter Array. We detected luminous HCN(1--0) emissions toward aconsiderable fraction of these Seyfert galaxies (10 of 12 in our sub-sample),which indicated that some of these Seyfert galaxies, such as NGC 3079, NGC3227, NGC 4051, NGC 6764, and NGC 7479, are indeed accompanied with compactnuclear starburst, given the tight correlation between the HCN(1--0) luminosityand the star formation rate among star-forming galaxies. However, we suggestthat the elevated HCN(1--0) emission from some of these Seyfert galaxies,including NGC 1068, NGC 1097, NGC 5033, and NGC 5194, does not signify thepresence of massive starbursts there. This is because these Seyfert nuclei showabnormally high HCN(1--0)/HCO$^+$(1--0) ratios (2--3), which were neverobserved in the starburst nuclei in our sample. This could be attributed to theoverabundance of HCN molecules in the X-ray dominated regions (XDRs) at thecenters of these Seyfert galaxies.


Instruction: what is the prompt that generates the input?

Input: Cornell University, the California Institute for Technology, and the JetPropulsion Laboratory are jointly studying the construction of a 25 m diametertelescope for submillimeter astronomy on a high mountain in northern Chile.This Cornell Caltech Atacama Telescope (CCAT) will combine high sensitivity, awide field of view, and a broad wavelength range to provide an unprecedentedcapability for deep, large area, multi-color submillimeter surveys tocomplement narrow field, high resolution studies with ALMA. CCAT observationswill address fundamental themes in contemporary astronomy, notably theformation and evolution of galaxies, the nature of the dark matter and darkenergy that comprise most of the content of the universe, the formation ofstars and planets, the conditions in circumstellar disks, and the conditionsduring the early history of the Solar system. The candidate CCAT site, at 5600m in northern Chile, enjoys superb observing conditions. To accommodate largeformat bolometer cameras, CCAT is designed with a 20 arcmin field of view. CCATwill incorporate closed loop active control of its segmented primary mirror tomaintain a half wavefront error of 10 mum rms or less. Instrumentation underconsideration includes both short (650 mum-200 mum) and long (2 mm-750 mum)wavelength bolometer cameras, direct detection spectrometers, and heterodynereceiver arrays. The University of Colorado, a Canadian university consortium,and the UK Astronomy Technology Centre on behalf of the UK community arepursuing participation in the CCAT consortium. When complete early in the nextdecade, CCAT will be the largest and most sensitive facility of its class aswell as the highest altitude astronomical facility on Earth.


Instruction: what is the prompt that generates the input?

Input: The Naval Research Laboratory and the National Radio Astronomy Observatorycompleted implementation of a low frequency capability on the VLA at 73.8 MHzin 1998. This frequency band offers unprecedented sensitivity (~25 mJy/beam)and resolution (~25 arcsec) for low-frequency observations. We review thehardware, the calibration and imaging strategies, comparing them to those athigher frequencies, including aspects of interference excision and wide-fieldimaging. Ionospheric phase fluctuations pose the major difficulty incalibrating the array. Over restricted fields of view or at times of extremelyquiescent ionospheric ``weather'', an angle-invariant calibration strategy canbe used. In this approach a single phase correction is devised for eachantenna, typically via self-calibration. Over larger fields of view or at timesof more normal ionospheric ``weather'' when the ionospheric isoplanatic patchsize is smaller than the field of view, we adopt a field-based strategy inwhich the phase correction depends upon location within the field of view. Thissecond calibration strategy was implemented by modeling the ionosphere abovethe array using Zernike polynomials. Images of 3C sources of moderate strengthare provided as examples of routine, angle-invariant calibration and imaging.Flux density measurements indicate that the 74 MHz flux scale at the VLA isstable to a few percent, and tied to the Baars et al. value of Cygnus A at the5 percent level. We also present an example of a wide-field image, devoid ofbright objects and containing hundreds of weaker sources, constructed from thefield-based calibration. We close with a summary of lessons the 74 MHz systemoffers as a model for new and developing low-frequency telescopes. (Abridged)


Instruction: what is the prompt that generates the input?

Input: Experimental studies have shown the ubiquity of altruistic behavior in humansocieties. The social structure is a fundamental ingredient to understand thedegree of altruism displayed by the members of a society, in contrast toindividual-based features, like for example age or gender, which have beenshown not to be relevant to determine the level of altruistic behavior. Weexplore an evolutionary model aiming to delve how altruistic behavior isaffected by social structure. We investigate the dynamics of interactingindividuals playing the Ultimatum Game with their neighbors given by a socialnetwork of interaction. We show that a population self-organizes in a criticalstate where the degree of altruism depends on the topology characterizing thesocial structure. In general, individuals offering large shares but in turnaccepting large shares, are removed from the population. In heterogeneoussocial networks, individuals offering intermediate shares are strongly selectedin contrast to random homogeneous networks where a broad range of offers, belowa critical one, is similarly present in the population.


Instruction: what is the prompt that generates the input?

Input: We present the results of the analysis of neutrino observations by theAntarctic Muon and Neutrino Detector Array (AMANDA) correlated with photonobservations of more than 400 gamma-ray bursts (GRBs) in the NorthernHemisphere from 1997 to 2003. During this time period, AMANDA's effectivecollection area for muon neutrinos was larger than that of any other existingdetector. Based on our observations of zero neutrinos during and immediatelyprior to the GRBs in the dataset, we set the most stringent upper limit on muonneutrino emission correlated with gamma-ray bursts. Assuming a Waxman-Bahcallspectrum and incorporating all systematic uncertainties, our flux upper limithas a normalization at 1 PeV of  E^2{\Phi}_{\nu} {\leq} 6.0 \times 10^{-9} GeV cm^{-2} s^{-1} sr^{-1}, with90% of the events expected within the energy range of ~10 TeV to ~3 PeV. Theimpact of this limit on several theoretical models of GRBs is discussed, aswell as the future potential for detection of GRBs by next generation neutrinotelescopes. Finally, we briefly describe several modifications to this analysisin order to apply it to other types of transient point sources.


Instruction: what is the prompt that generates the input?

Input: The churn rate of a peer-to-peer system places direct limitations on the rateat which messages can be effectively communicated to a group of peers. Theselimitations are independent of the topology and message transmission latency.In this paper we consider a peer-to-peer network, based on the Engset model,where peers arrive and depart independently at random. We show how the arrivaland departure rates directly limit the capacity for message streams to bebroadcast to all other peers, by deriving mean field models that accuratelydescribe the system behavior. Our models cover the unit and more general kbuffer cases, i.e. where a peer can buffer at most k messages at any one time,and we give results for both single and multi-source message streams. We definecoverage rate as peer-messages per unit time, i.e. the rate at which a numberof peers receive messages, and show that the coverage rate is limited by thechurn rate and buffer size. Our theory introduces an Instantaneous MessageExchange (IME) model and provides a template for further analysis of morecomplicated systems. Using the IME model, and assuming random processes, wehave obtained very accurate equations of the system dynamics in a variety ofinteresting cases, that allow us to tune a peer-to-peer system. It remains tobe seen if we can maintain this accuracy for general processes and whenapplying a non-instantaneous model.


Instruction: what is the prompt that generates the input?

Input: The cosmological redshift phenomenon can be described by the dark matterfield fluid model, the results deduced from this model agree very well with theobservations. The observed cosmological redshift of light depends on both thespeed of the emitter and the distance between the emitter and the observer. Ifthe emitter moves away from us, a redshift is observed. If the emitter movestowards us, whether a redshift, a blueshift or no shift is observed will dependon the speed vs. the distance. If the speed is in the range ofc(exp[-beta*D]-1) < v < 0, a redshift is observed; if the speed equalsc(exp[-beta*D]-1), no shift is observed; if the speed v less thanc(exp[-beta*D]-1), a blueshift is observed. A redshift will be always observedin all directions for any celestial objects as long as their distance from usis large enough. Therefore, many more redshifts than blueshifts should beobserved for galaxies and supernovae, etc in the sky. This conclusion agreeswith current observations. The estimated value of the redshift constant beta ofthe dark matter field fluid is in the range of 10^(-3) ~ 10^(-5)/Mpc. A largeredshift value from a distant celestial object may not necessarily indicatethat it has a large receding speed. Based on the redshift effect of dark matterfield fluid, it is concluded that at least in time average all photons have thesame geometry (size and shape) in all inertial reference frames and do not havelength contraction effect.


Instruction: what is the prompt that generates the input?

Input: Redundancy of experimental data is the basic statistic from which thecomplexity of a natural phenomenon and the proper number of experiments neededfor its exploration can be estimated. The redundancy is expressed by theentropy of information pertaining to the probability density function ofexperimental variables. Since the calculation of entropy is inconvenient due tointegration over a range of variables, an approximate expression for redundancyis derived that includes only a sum over the set of experimental data aboutthese variables. The approximation makes feasible an efficient estimation ofthe redundancy of data along with the related experimental information andinformation cost function. From the experimental information the complexity ofthe phenomenon can be simply estimated, while the proper number of experimentsneeded for its exploration can be determined from the minimum of the costfunction. The performance of the approximate estimation of these statistics isdemonstrated on two-dimensional normally distributed random data.


Instruction: what is the prompt that generates the input?

Input: Finite metric trees are known to have strict 1-negative type. In this paperwe introduce a new family of inequalities that quantify the extent of the"strictness" of the 1-negative type inequalities for finite metric trees. Theseinequalities of "enhanced 1-negative type" are sufficiently strong to implythat any given finite metric tree must have strict p-negative type for allvalues of p in an open interval that contains the number 1. Moreover, theseopen intervals can be characterized purely in terms of the unordereddistribution of edge weights that determine the path metric on the particulartree, and are therefore largely independent of the tree's internal geometry.  From these calculations we are able to extract a new non linear technique forimproving lower bounds on the maximal p-negative type of certain finite metricspaces. Some pathological examples are also considered in order to stresscertain technical points.


Instruction: what is the prompt that generates the input?

Input: This paper focuses on the kinematic properties of a newthree-degree-of-freedom hybrid manipulator. This manipulator is obtained byadding in series to a five-bar planar mechanism (similar to the one studied byBajpai and Roth) a third revolute passing through the line of centers of thetwo actuated revolute joints of the above linkage. The resulting architectureis hybrid in that it has both serial and parallel links. Fully-parallelmanipulators are known for the existence of particularly undesirablesingularities (referred to as parallel singularities) where control is lost [4]and [6]. On the other hand, due to their cantilever type of kinematicarrangement, fully serial manipulators suffer from a lack of stiffness and fromrelatively large positioning errors. The hybrid manipulator studied isintrinsically stiffer and more accurate. Furthermore, since all actuators arelocated on the first axis, the inertial effects are considerably reduced. Inaddition, it is shown that the special kinematic structure of our manipulatorhas the potential of avoiding parallel singularities by a suitable choice ofthe "working mode", thus leading to larger workspaces. The influence of thedifferent structural dimensions (e.g. the link lengths) on the kinematic andmechanical properties are analysed in view of the optimal design of such hybridmanipulators.


Instruction: what is the prompt that generates the input?

Input: In 1929 Heisenberg and Pauli laid the foundations of QFT by quantizing thefields (method of canonical quantization). This general theory of quantizedfields has remained undisputed up to now. We show how the unmodifiedHeisenberg-Pauli calculations make sense mathematically by using a theory ofgeneralized functions adapted to nonlinear operations. By providing anappropriate mathematical setting, nonlinear generalized functions open doorsfor their understanding but there remains presumably very hard technicalproblems. (i) Domains of the interacting field operators: a priori the H-Pcalculations give time dependent dense domains, what is not very convenient;(ii) Calculations of the resulting matrix elements of the S operator: from theunitarity of the S operator as a whole there are no longer ``infinities,'' buta priori there is no other hope than heavy computer calculations; (iii)Connection with renormalization theory: it should provide an approximation whenthe coupling constant is small. The aim of this paper is to present, on thegrounds of a standard mathematical model of QFT (a self interacting scalarboson field), a basis for improvement without significant prerequisites inmathematics and physics. It is an attempt to use nonlinear generalizedfunctions in QFT, starting directly from the calculations made by physicists,in the same way as they have already been used in classical mechanics andgeneral relativity.


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Input: In this paper, the notion of {\em $p$-adic multiresolution analysis (MRA)} isintroduced. We use a ``natural'' refinement equation whose solution (arefinable function) is the characteristic function of the unit disc. Thisequation reflects the fact that the characteristic function of the unit disc isthe sum of $p$ characteristic functions of disjoint discs of radius $p^{-1}$.The case $p=2$ is studied in detail. Our MRA is a 2-adic analog of the realHaar MRA. But in contrast to the real setting, the refinable functiongenerating our Haar MRA is periodic with period 1, which never holds for realrefinable functions. This fact implies that there exist infinity many different2-adic orthonormal wavelet bases in ${\cL}^2(\bQ_2)$ generated by the same HaarMRA. All of these bases are constructed. Since $p$-adic pseudo-differentialoperators are closely related to wavelet-type bases, our bases can beintensively used for applications.


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Input: A rotating bosonic many-body system in a harmonic trap is studied with the3D-Cranked Hartree-Fock-Bogoliubov method at zero temperature, which has beenapplied to nuclear many-body systems at high spin. This method is a variationalmethod extended from the Hartree-Fock theory, which can treat the pairingcorrelations in a self-consistent manner. An advantage of this method is that afinite-range interaction between constituent particles can be used in thecalculation, unlike the original Gross-Pitaevskii approach. To demonstrate thevalidity of our method, we present a calculation for a toy model, that is, arotating system of ten bosonic particles interacting through the repulsivequadrupole-quadrupole interaction in a harmonic trap. It is found that theyrast states, the lowest-energy states for the given total angular momentum,does not correspond to the Bose-Einstein condensate, except a few specialcases. One of such cases is a vortex state, which appears when the totalangular momentum $L$ is twice the particle number $N$ (i.e., $L=2N$).


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Input: Through polarization observations masers are unique probes of the magneticfield in a variety of different astronomical objects, with the different maserspecies tracing different physical conditions. In recent years maserpolarization observations have provided insights in the magnetic field strengthand morphology in, among others, the envelopes around evolved stars, PlanetaryNebulae (PNe), massive star forming regions and supernova remnants. Morerecently, maser observations have even been used to determine the magneticfield in megamaser galaxies. This review will present an overview of maserpolarization observations and magnetic field determinations of the last severalyears and discuss the implications of the magnetic field measurements forseveral important fields of study, such as aspherical PNe creation and massivestar formation.


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Input: The existence of neutrino masses strongly suggests that right-handedneutrinos exist, but the data do not favor any particular scale for theMajorana mass parameters. Here I explore the possibility that these particlesexist at the electroweak scale along with additional new physics at the TeVscale . Higher dimension operators involving right-handed neutrinos and theHiggs boson can introduce new decay modes of the Higgs boson, significantlymodifying its phenomenology if it is light. With minimal flavor violation theHiggs boson cascade decays to 6 particles containing two highly displacedvertices. Each displaced vertex produces an odd number of leptons, leading to adramatic signature of overall lepton violation at each vertex. I discuss thelimits from the Tevatron, and find that they are close to exploring interestingregions of parameters, while limiting others. Moving beyond minimal flavorviolation, cascade decays of the Higgs boson into as many as 14 particles canoccur.


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Input: Surface roughness becomes relevant if typical length scales of the system arecomparable to the scale of the variations as it is the case in microfluidicsetups. Here, an apparent boundary slip is often detected which can have itsorigin in the assumption of perfectly smooth boundaries. We investigate theproblem by means of lattice Boltzmann (LB) simulations and introduce an``effective no-slip plane'' at an intermediate position between peaks andvalleys of the surface. Our simulations show good agreement with analyticalresults for sinusoidal boundaries, but can be extended to arbitrary geometriesand experimentally obtained surface data. We find that the detected apparentslip is independent of the detailed boundary shape, but only given by thedistribution of surface heights. Further, we show that the slip diverges as theamplitude of the roughness increases.


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Input: We show that hard-scattering factorization is violated in the production ofhigh-p_T hadrons in hadron-hadron collisions, in the case that the hadrons areback-to-back, so that k_T factorization is to be used. The explicitcounterexample that we construct is for the single-spin asymmetry with one beamtransversely polarized. The Sivers function needed here has particularsensitivity to the Wilson lines in the parton densities. We use a greatlysimplified model theory to make the breakdown of factorization easy to checkexplicitly. But the counterexample implies that standard arguments forfactorization fail not just for the single-spin asymmetry but for theunpolarized cross section for back-to-back hadron production in QCD inhadron-hadron collisions. This is unlike corresponding cases in e^+e^-annihilation, Drell-Yan, and deeply inelastic scattering. Moreover, the resultendangers factorization for more general hadroproduction processes.


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Input: We study the dc conductance of organic single-molecule contacts in thepresence of external electromagnetic radiation (photoconductance). In agreementwith previous predictions, we find that the radiation can lead to largeenhancements of the conductance of such contacts by bringing off-resonantlevels into resonance through photoassisted processes. In our analysis we makeuse of the simplifying fact that, under certain assumptions, thephotoconductance can be expressed in terms of the transmission function in theabsence of the radiation. The conductance enhancement is demonstrated foroligophenylene molecules between gold electrodes, whose electronic structure iscalculated based on density-functional theory. It is shown that the exponentialdecay of the conductance with the length of the molecule can be replaced by alength-independent value in the presence of radiation.


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Input: As the dimensionality is reduced, the world becomes more and moreinteresting; novel and fascinating phenomena show up which call forunderstanding. Physics in one dimension is a fascinating topic for theory andexperiment: for the former often a simplification, for the latter always achallenge. Various ways will be demonstrated how one-dimensional structures canbe achieved in reality. In particular organic conductors could establishthemselves as model systems for the investigation of the physics in reduceddimensions.  In the metallic state of a one-dimensional solid, Fermi-liquid theory breaksdown and spin and charge degrees of freedom become separated. But the metallicphase is not stable in one dimension: as the temperature is reduced, theelectronic charge and spin tend to arrange themselves in an ordered fashion dueto strong correlations. The competition of the different interactions isresponsible for which broken-symmetry ground state is eventually realized in aspecific compound and which drives the system towards an insulating state.  Here we review the various ordering phenomena and how they can be identifiedby dielectric and optic measurements.


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Input: In the framework of the model inter-comparison study - Asia Phase II (MICS2),where eight models are compared over East Asia, this paper studies theinfluence of different parameterizations used in the aerosol module on theaerosol concentrations of sulfate and nitrate in PM10. An intracomparison ofaerosol concentrations is done for March 2001 using different configurations ofthe aerosol module of one of the model used for the intercomparison. Singlemodifications of a reference setup for model configurations are performed andcompared to a reference case. These modifications concern the sizedistribution, i.e. the number of sections, and physical processes, i.e.coagulation, condensation/evaporation, cloud chemistry, heterogeneous reactionsand sea-salt emissions. Comparing monthly averaged concentrations at differentstations, the importance of each parameterization is first assessed. It isfound that sulfate concentrations are little sensitive to sea-salt emissionsand to whether condensation is computed dynamically or by assumingthermodynamic equilibrium. Nitrate concentrations are little sensitive to cloudchemistry. However, a very high sensitivity to heterogeneous reactions isobserved. Thereafter, the variability of the aerosol concentrations to the useof different chemistry transport models (CTMs) and the variability to the useof different parameterizations in the aerosol module are compared. For sulfate,the variability to the use of different parameterizations in the aerosol moduleis lower than the variability to the use of different CTMs. However, fornitrate, for monthly averaged concentrations averaged over four stations, thesetwo variabilities have the same order of magnitude.


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Input: This paper introduces a continuous model for Multi-cellular DevelopmentalDesign. The cells are fixed on a 2D grid and exchange "chemicals" with theirneighbors during the growth process. The quantity of chemicals that a cellproduces, as well as the differentiation value of the cell in the phenotype,are controlled by a Neural Network (the genotype) that takes as inputs thechemicals produced by the neighboring cells at the previous time step. In theproposed model, the number of iterations of the growth process is notpre-determined, but emerges during evolution: only organisms for which thegrowth process stabilizes give a phenotype (the stable state), others aredeclared nonviable. The optimization of the controller is done using the NEATalgorithm, that optimizes both the topology and the weights of the NeuralNetworks. Though each cell only receives local information from its neighbors,the experimental results of the proposed approach on the 'flags' problems (thephenotype must match a given 2D pattern) are almost as good as those of adirect regression approach using the same model with global information.Moreover, the resulting multi-cellular organisms exhibit almost perfectself-healing characteristics.


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Input: Cold dark matter haloes are populated by caustics, which are yet to beresolved in N-body simulations or observed in the Universe. Secondary infallmodel provides a paradigm for the study of caustics in "typical" haloesassuming that they have had no major mergers and have grown only by smoothaccretion. This is a particular characteristic of the smallest dark matterhaloes of about 10^{-5} Mo, which although "atypical" contain no substructuresand could have survived until now with no major mergers. Thus using this modelas the first guidline, we evaluate the neutralino self-annihilation flux forthese haloes. Our results show that caustics could leave a distinct sawteethsignature on the differential and cumulative fluxes coming from the outerregions of these haloes. The total annihilation signal from the regions awayfrom the centre can be boosted by about forty percents.


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Input: A long standing problem is the supergauge completion of AdS_4 x (G/H)_7 orAdS_5 x (G/H)_5 backgrounds which preserve less then maximal supersymmetry. Inparallel with the supersolvable realization of the AdS_4 x S^7 background basedon Kappa-symmetry, we develop a technique which amounts to solving theabove-mentioned problem in a way useful for pure spinor quantization forsupermembranes and superstrings. Instead of gauge fixing some of the superspacecoordinates to zero, we impose an additional constraint on them reproducing thesimplifications of the supersolvable representations. The constraints arequadratic, homogeneous, Sp(4,R)-covariant, and consistent from the quantumpoint of view in the pure spinor approach. Here we provide the geometricalsolution which, in a subsequent work, will be applied to the membrane and thesuperstring sigma models.


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Input: We present spectroscopic observations of 11 moderately high-redshift (z~0.7-1.0) clusters from the first Red-Sequence Cluster Survey (RCS-1). We findexcellent agreement between the red-sequence estimated redshift and thespectroscopic redshift, with a scatter of 10% at z>0.7. At the high-redshiftend (z>~0.9) of the sample, we find two of the systems selected are projectionsof pairs of comparably rich systems, with red-sequences too close todiscriminate in (R-z') colour. In one of these systems, the two components areclose enough to be physically associated. For a subsample of clusters withsufficient spectroscopic members, we examine the correlation between B_gcR(optical richness) and the dynamical mass inferred from the velocitydispersion. We find these measurements to be compatible, within the relativelylarge uncertainties, with the correlation established at lower redshift for theX-ray selected CNOC1 clusters and also for a lower redshift sample of RCS-1clusters. Confirmation of this and calibration of the scatter in the relationwill require larger samples of clusters at these and higher redshifts.[abridged]


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Input: [Abridged] We test the accuracy of different models of the attenuation oflight due to resonant scattering by intergalactic neutral hydrogen by comparingtheir predictions of the evolution of the mean cosmic flux decrement, D_A, tomeasurements of this quantity based on observations. To this end, we use dataavailable in the literature and our own measurements of the cosmic fluxdecrement for 25 quasars in the redshift range 2.71 < z < 5.41 taken from theSDSS Data Release 5. In order to perform the measurements of D_A, we fit apower-law to the continuum redward of the Lya emission line, and extrapolatethis fit to region blueward of it, where the flux is severely affected byabsorption due to intervening HI absorbers. We compute, using numericalsimulations, the redshift evolution of D_A accounting for the presence of LyaForest absorbers and Lyman limit systems randomly distributed along theline-of-sight, and compute its intrinsic scatter at the 1-, 2-, and 3-sigmalevel due to fluctuations in the absorber properties (column density, Dopplerparameter, redshift) along different lines-of-sight. The numerical simulationsconsist of Monte Carlo realizations of distributions of the absorber propertiesconstrained from observations. The results from the models considered hereconfirm our theoretical expectation that the distribution of D_A at any givenredshift be well described by a lognormal distribution function. This impliesthat the effective optical depth, usually defined as the negative logarithm ofthe average flux, 1 - D_A, is very accurately Gaussian distributed, in contrastto previous studies. This result is independent to the form of the inputdistribution functions, and rather insensitive to the presence of high-columndensity absorbers, such as the Lyman limit systems.


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Input: The bipolar HH 212 outflow has been mapped in SiO using the extendedconfiguration of the Plateau de Bure Interferometer (PdBI), revealing a highlycollimated SiO jet closely associated with the H2 jet component. We study atunprecedented resolution (0.34" across the jet axis) the properties of theinnermost SiO ``microjet'' within 1000 AU of this young Class 0 source, tocompare it with atomic microjets from more evolved sources and to constrain itsorigin. The SiO channel maps are used to investigate the microjet collimationand velocity structure. A large velocity gradient analysis is applied to SiO(2-1), (5-4) and (8-7) data from the PdBI and the Submillimeter Array toconstrain the SiO opacity and abundance. The HH212 Class 0 microjet showsstriking similarities in collimation and energetic budget with atomic microjetsfrom T Tauri sources. Furthermore, the SiO lines appear optically thick, unlikewhat is generally assumed. We infer T(kin) ~ 50-500 K and an SiO/H2 abundancegreater than 4 10(-8)-6 10(-5) for n(H2) = 10(7)-10(5) cm(-3), i.e. 0.05-90% ofthe elemental silicon. This similar jet width, regardless of the presence of adense envelope, definitely rules out jet collimation by external pressure, andfavors a common MHD self-collimation (and possibly acceleration) process at allstages of star formation. We propose that the more abundant SiO in Class 0 jetscould mainly result from rapid (less than 25 yrs) molecular synthesis at highjet densities.


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Input: The temperature variation effect of shape anisotropy on the coercivity,HC(T), for the aligned Stoner-Wohlfarth (SW) soft ferromagnets, such as fcc Ni,fcc Co and bcc Fe, are investigated within the framework of Neel-Brown (N-B)analysis. An extended N-B equation is thus proposed,by introducing a singledimensionless correction function, the reduced magnetization, m(\tao) =MS(T)/MS(0), in which \tao = T/TC is the reduced temperature, MS(T) is thesaturation magnetization, and TC is the Curie temperature. The factor, m(\tao),accounts for the temperature-dependent effect of the shape anisotropy. Theconstants, H0 and E0, are for the switching field at zero temperature and thepotential barrier at zero field, respectively. According to this newly derivedequation, the blocking temperature above which the properties ofsuperparamagnetism show up is described by the expression, TB =E0m^2(\tao)/[kBln(t/t0)], with the extra correction factor m^2(\tao). Thepossible effect on HC(T) and the blocking temperature, TB, attributed to thedownshift of TC resulting from the finite size effect has been discussed also.


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Input: We present an analysis of the Lyman alpha forests of five quasar spectra inthe near UV. Properties of the intergalactic medium (IGM) at an intermediateredshift interval (0.9 < z < 1.9) are studied. The amount of baryons in thediffuse photoionised IGM and the warm-hot intergalactic medium (WHIM) aretraced to get constraints on the redshift evolution of the different phases ofthe intergalactic gas. The baryon density of the diffuse IGM is determined withphotoionisation calculations under the assumption of local hydrostaticequilibrium. We assume that the gas is ionised by a metagalactic backgroundradiation with a Haardt & Madau (2001) spectrum. The WHIM is traced with broadLyman alpha (BLA) absorption. The properties of a number of BLA detections arestudied. Under the assumption of collisional ionisation equilibrium a lowerlimit to the baryon density could be estimated. It is found that the diffusephotoionised IGM contains at least 25% of the total baryonic matter atredshifts 1 < z < 2. For the WHIM a lower limit of 2.4% could be determined.Furthermore the data indicates that the intergalactic gas is in a state ofevolution at z=1.5. We confirm that a considerable part of the WHIM is createdbetween z=1 and z=2.


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Input: Consider the partition function of a directed polymer in an IID field. Weassume that both tails of the negative and the positive part of the field areat least as light as exponential. It is a well-known fact that the free energyof the polymer is equal to a deterministic constant for almost everyrealization of the field and that the upper tail of the large deviations isexponential. The lower tail of the large deviations is typically lighter thanexponential. In this paper we provide a method to obtain estimates on the rateof decay of the lower tail of the large deviations, which are sharp up tomultiplicative constants. As a consequence, we show that the lower tail of thelarge deviations exhibits three regimes, determined according to the tail ofthe negative part of the field. Our method is simple to apply and can be usedto cover other oriented and non-oriented models including first/last-passagepercolation and the parabolic Anderson model


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Input: Utilizing an eigenfunction decomposition, we study the growth and spectra ofenergy in the vortical and wave modes of a 3D rotating stratified fluid as afunction of $\epsilon = f/N$. Working in regimes characterized by moderateBurger numbers, i.e. $Bu = 1/\epsilon^2 < 1$ or $Bu \ge 1$, our resultsindicate profound change in the character of vortical and wave modeinteractions with respect to $Bu = 1$. As with the reference state of$\epsilon=1$, for $\epsilon < 1$ the wave mode energy saturates quite quicklyand the ensuing forward cascade continues to act as an efficient means ofdissipating ageostrophic energy. Further, these saturated spectra steepen as$\epsilon$ decreases: we see a shift from $k^{-1}$ to $k^{-5/3}$ scaling for$k_f < k < k_d$ (where $k_f$ and $k_d$ are the forcing and dissipation scales,respectively). On the other hand, when $\epsilon > 1$ the wave mode energynever saturates and comes to dominate the total energy in the system. In fact,in a sense the wave modes behave in an asymmetric manner about $\epsilon = 1$.With regard to the vortical modes, for $\epsilon \le 1$, the signatures of 3Dquasigeostrophy are clearly evident. Specifically, we see a $k^{-3}$ scalingfor $k_f < k < k_d$ and, in accord with an inverse transfer of energy, thevortical mode energy never saturates but rather increases for all $k < k_f$. Incontrast, for $\epsilon > 1$ and increasing, the vortical modes contain aprogressively smaller fraction of the total energy indicating that the 3Dquasigeostrophic subsystem plays an energetically smaller role in the overalldynamics.


Instruction: what is the prompt that generates the input?

Input: A series of semi-inclusive deep-inelastic scattering measurements ondeuterium, helium, neon, krypton, and xenon targets has been performed in orderto study hadronization. The data were collected with the HERMES detector at theDESY laboratory using a 27.6 GeV positron or electron beam. Hadronmultiplicities on nucleus A relative to those on the deuteron, R_A^h, arepresented for various hadrons (\pi^+, \pi^-, \pi^0, K^+, K^-, p, and \bar{p})as a function of the virtual-photon energy \nu, the fraction z of this energytransferred to the hadron, the photon virtuality Q^2, and the hadron transversemomentum squared p_t^2. The data reveal a systematic decrease of R_A^h with themass number A for each hadron type h. Furthermore, R_A^h increases (decreases)with increasing values of \nu (z), increases slightly with increasing Q^2, andis almost independent of p_t^2, except at large values of p_t^2. For pionstwo-dimensional distributions also are presented. These indicate that thedependences of R_A^{\pi} on \nu and z can largely be described as a dependenceon a single variable L_c, which is a combination of \nu and z. The dependenceon L_c suggests in which kinematic conditions partonic and hadronic mechanismsmay be dominant. The behaviour of R_A^{\pi} at large p_t^2 constitutestentative evidence for a partonic energy-loss mechanism. The A-dependence ofR_A^h is investigated as a function of \nu, z, and of L_c. It approximatelyfollows an A^{\alpha} form with \alpha \approx 0.5 - 0.6.