Instruction: what is the prompt that generates the input?

Input: We present predictions for the evolution of the galaxy luminosity function,number counts and redshift distributions in the IR based on the Lambda-CDMcosmological model. We use the combined GALFORM semi-analytical galaxyformation model and GRASIL spectrophotometric code to compute galaxy SEDsincluding the reprocessing of radiation by dust. The model, which is the sameas that in Baugh et al (2005), assumes two different IMFs: a normal solarneighbourhood IMF for quiescent star formation in disks, and a very top-heavyIMF in starbursts triggered by galaxy mergers. We have shown previously thatthe top-heavy IMF seems to be necessary to explain the number counts of faintsub-mm galaxies. We compare the model with observational data from the SPITZERSpace Telescope, with the model parameters fixed at values chosen beforeSPITZER data became available. We find that the model matches the observedevolution in the IR remarkably well over the whole range of wavelengths probedby SPITZER. In particular, the SPITZER data show that there is strong evolutionin the mid-IR galaxy luminosity function over the redshift range z ~ 0-2, andthis is reproduced by our model without requiring any adjustment of parameters.On the other hand, a model with a normal IMF in starbursts predicts far toolittle evolution in the mid-IR luminosity function, and is therefore excluded.


Instruction: what is the prompt that generates the input?

Input: We present results of the analysis of cometary X-ray spectra with an extendedversion of our charge exchange emission model (Bodewits et al. 2006). We haveapplied this model to the sample of 8 comets thus far observed with the ChandraX-ray observatory and ACIS spectrometer in the 300-1000 eV range. The surveyedcomets are C/1999 S4 (LINEAR), C/1999 T1 (McNaught-Hartley), C/2000 WM1(LINEAR), 153P/2002 (Ikeya-Zhang), 2P/2003 (Encke), C/2001 Q4 (NEAT), 9P/2005(Tempel 1) and 73P/2006-B (Schwassmann-Wachmann 3) and the observations includea broad variety of comets, solar wind environments and observationalconditions. The interaction model is based on state selective, velocitydependent charge exchange cross sections and is used to explore how cometaryX-ray emission depend on cometary, observational and solar windcharacteristics. It is further demonstrated that cometary X-ray spectra mainlyreflect the state of the local solar wind. The current sample of Chandraobservations was fit using the constrains of the charge exchange model, andrelative solar wind abundances were derived from the X-ray spectra. Ouranalysis showed that spectral differences can be ascribed to different solarwind states, as such identifying comets interacting with (I) fast, cold wind,(II), slow, warm wind and (III) disturbed, fast, hot winds associated withinterplanetary coronal mass ejections. We furthermore predict the existence ofa fourth spectral class, associated with the cool, fast high latitude wind.


Instruction: what is the prompt that generates the input?

Input: Surviving in a diverse environment requires corresponding organism responses.At the cellular level, such adjustment relies on the transcription factors(TFs) which must rapidly find their target sequences amidst a vast amount ofnon-relevant sequences on DNA molecules. Whether these transcription factorslocate their target sites through a 1D or 3D pathway is still a matter ofspeculation. It has been suggested that the optimum search time is when theprotein equally shares its search time between 1D and 3D diffusions. In thispaper, we study the above problem using a Monte Carlo simulation by consideringa very simple physical model. A 1D strip, representing a DNA, with a number oflow affinity sites, corresponding to non-target sites, and high affinity sites,corresponding to target sites, is considered and later extended to a 2D strip.We study the 1D and 3D exploration pathways, and combinations of the two modesby considering three different types of molecules: a walker that randomly walksalong the strip with no dissociation; a jumper that represents dissociation andthen re-association of a TF with the strip at later time at a distant site; anda hopper that is similar to the jumper but it dissociates and thenre-associates at a faster rate than the jumper. We analyze the finalprobability distribution of molecules for each case and find that TFs canlocate their targets fast enough even if they spend 15% of their search timediffusing freely in the solution. This indeed agrees with recent experimentalresults obtained by Elf et al. 2007 and is in contrast with theoreticalexpectation.


Instruction: what is the prompt that generates the input?

Input: We examine the structure of the post-shock region in supernova remnants(SNRs). The ``shock transition zone'' is set up by charge transfer andionization events between atoms and ions, and has a width $\sim 10^{15}$cm$^{-2}$ $n^{-1}_0$, where $n_0$ is the total pre-shock density (includingboth atoms and ions). For Balmer-dominated SNRs with shock velocity $v_s\gtrsim 1000$ km s$^{-1}$, the Rankine-Hugoniot conditions for ion velocity andtemperature are obeyed instantly, leaving the full width at half-maximum (FWHM)of the broad H$\alpha$ line versus $v_s$ relation intact. However, the spatialvariation in the post-shock densities is relevant to the problem of Ly$\alpha$resonant scattering in young, core-collapse SNRs. Both two- (pre-shock atomsand ions) and three-component (pre-shock atoms, broad neutrals and ions) modelsare considered. We compute the spatial emissivities of the broad ($\xi_b$) andnarrow ($\xi_n$) H$\alpha$ lines; a calculation of these emissivities in SN1006 is in general agreement with the computed ones of Raymond et al. (2007).The (dimensionless) spatial shift, $\Theta_{\rm{shift}}$, between the centroidsof $\xi_b$ and $\xi_n$ is unique for a given shock velocity and $f_{\rm{ion}}$,the pre-shock ion fraction. Measurements of $\Theta_{\rm{shift}}$ can be usedto constrain $n_0$.


Instruction: what is the prompt that generates the input?

Input: Clear evidence for symplectic symmetry in low-lying states of $^{12}$C and$^{16}$O is reported. Eigenstates of $^{12}$C and $^{16}$O, determined withinthe framework of the no-core shell model using the JISP16 $NN$ realisticinteraction, typically project at the 85-90% level onto a few of the mostdeformed symplectic basis states that span only a small fraction of the fullmodel space. The results are nearly independent of whether the bare orrenormalized effective interactions are used in the analysis. The outcomeconfirms Elliott's \SU{3} model which underpins the symplectic scheme, andabove all, points to the relevance of a symplectic no-core shell model that canreproduce experimental B(E2) values without effective charges as well asdeformed spatial modes associated with clustering phenomena in nuclei.


Instruction: what is the prompt that generates the input?

Input: We use strongly coupled lattice QED with two flavors of massless staggeredfermions to model the physics of pions in two-flavor massless QCD. Our modelhas the right chiral symmetries and can be studied efficiently with clusteralgorithms. In particular we can tune the strength of the QCD anomaly and thusstudy its effects on the chiral phase transition. Our study confirms the widelyaccepted view point that the chiral phase transition is first order in theabsence of the anomaly. Turning on the anomaly weakens the transition and turnsit second order at a critical anomaly strength. The anomaly strength at thetricritical point is characterized using $r = (M_{\eta'}-M_{\pi})/\rho_{\eta'}$where $M_{\eta'}, M_{\pi}$ are the screening masses of the anomalous andregular pions and $\rho_{\eta'}$ is the mass-scale that governs the low energyfluctuations of the anomalous symmetry. We estimate that $r \sim 7 $ in ourmodel. This suggests that a strong anomaly at the two-flavor QCD chiral phasetransition is necessary to wash out the first order transition.


Instruction: what is the prompt that generates the input?

Input: By making use of the finite-temperature real-time static potential that wasintroduced and computed to leading non-trivial order in Hard Thermal Loopresummed perturbation theory in recent work, and solving numerically aSchr\"odinger-type equation, we estimate the quarkonium (in practice,bottomonium) contribution to the spectral function of the electromagneticcurrent in hot QCD. The spectral function shows a single resonance peak whichbecomes wider and then disappears as the temperature is increased beyond 450MeV or so. This behaviour can be compared with recently attempted latticereconstructions of the same quantity, based on the ``maximum entropy method'',which generically show several peaks. We also specify the dependence of ourresults on the spatial momentum of the electromagnetic current, as well as onthe baryon chemical potential characterising the hot QCD plasma.


Instruction: what is the prompt that generates the input?

Input: We study the infrared (IR) properties of galaxies in the cluster MS 1054-03at z=0.83 by combining MIPS 24 micron data with spectra of more than 400galaxies and a very deep K-band selected catalog. 19 IR cluster members areselected spectroscopically, and an additional 15 are selected by theirphotometric redshifts. We derive the IR luminosity function of the cluster andfind strong evolution compared to the similar-mass Coma cluster. The bestfitting Schechter function gives L*_{IR}=11.49 +0.30/-0.29 L_sun with a fixedfaint end slope, about one order of magnitude larger than that in Coma. Therate of evolution of the IR luminosity from Coma to MS 1054-03 is consistentwith that found in field galaxies, and it suggests that some internalmechanism, e.g., the consumption of the gas fuel, is responsible for thegeneral decline of the cosmic star formation rate (SFR) in differentenvironments. The mass-normalized integrated SFR within 0.5R_200 in MS 1054-03also shows evolution compared with other rich clusters at lower redshifts, butthe trend is less conclusive if the mass selection effect is considered. Anonnegligible fraction (13%) of cluster members, are forming stars actively andthe overdensity of IR galaxies is about 20 compared to the field. It isunlikely that clusters only passively accrete star forming galaxies from thesurrounding fields and have their star formation quenched quickly afterward;instead, many cluster galaxies still have large amounts of gas, and their starformation may be enhanced by the interaction with the cluster.


Instruction: what is the prompt that generates the input?

Input: The X-ray transient XMMU J174716.1-281048 was serendipitously discovered withXMM-Newton in 2003. It lies about 0.9 degrees off the Galactic Centre and itsspectrum shows a high absorption (~8 x 10E22 cm^(-2)). Previous X-rayobservations of the source field performed in 2000 and 2001 did not detect thesource, indicative of a quiescent emission at least two orders of magnitudefainter. The low luminosity during the outburst (~5 x 10E34 erg/s at 8 kpc)indicates that the source is a member of the ``very faint X-ray transients''class. On 2005 March 22nd the INTEGRAL satellite caught a possible type-I X-rayburst from the new INTEGRAL source IGR J17464-2811, classified as fast X-raytransient. This source was soon found to be positionally coincident, within theuncertainties, with XMMU J174716.1-281048. Here we report data analysis of theX-ray burst observed with the IBIS and JEM-X telescopes and confirm the type-Iburst nature. We also re-analysed XMM-Newton and Chandra archival observationsof the source field. We discuss the implications of these new findings,particularly related to the source distance as well as the sourceclassification.


Instruction: what is the prompt that generates the input?

Input: The phase of Super-Soft-Source (SSS) emission of the sixth recorded outburstof the recurrent nova RS Oph was observed twice with Chandra and once withXMM-Newton. The observations were taken on days 39.7, 54.0, and 66.9 afteroutburst. We confirm a 35-sec period on day 54.0 and found that it originatesfrom the SSS emission and not from the shock. We discus the bound-freeabsorption by neutral elements in the line of sight, resonance absorption linesplus self-absorbed emission line components, collisionally excited emissionlines from the shock, He-like intersystem lines, and spectral changes during anepisode of high-amplitude variability. We find a decrease of the oxygen K-shellabsorption edge that can be explained by photoionization of oxygen. Theabsorption component has average velocities of -1286+-267 km/s on day 39.7 andof -771+-65 km/s on day 66.9. The wavelengths of the emission line componentsare consistent with their rest wavelengths as confirmed by measurements ofnon-self absorbed He-like intersystem lines. We have evidence that these linesoriginate from the shock rather than the outer layers of the outflow and may bephotoexcited in addition to collisional excitations. We found collisionallyexcited emission lines that are fading at wavelengths shorter than 15A thatoriginate from the radiatively cooling shock. On day 39.5 we find a systematicblue shift of -526+-114 km/s from these lines. We found anomalous He-like f/iratios which indicates either high densities or significant UV radiation nearthe plasma where the emission lines are formed. During the phase of strongvariability the spectral hardness light curve overlies the total light curvewhen shifted by 1000sec. This can be explained by photoionization of neutraloxygen in the line of sight if the densities of order 10^{10}-10^{11} cm^{-3}.


Instruction: what is the prompt that generates the input?

Input: A coarse-grained computational procedure based on the Finite Element Methodis proposed to calculate the normal modes and mechanical response of proteinsand their supramolecular assemblies. Motivated by the elastic network model,proteins are modeled as homogeneous isotropic elastic solids with volumedefined by their solvent-excluded surface. The discretized Finite Elementrepresentation is obtained using a surface simplification algorithm thatfacilitates the generation of models of arbitrary prescribed spatialresolution. The procedure is applied to compute the normal modes of a mutant ofT4 phage lysozyme and of filamentous actin, as well as the critical Eulerbuckling load of the latter when subject to axial compression. Results comparefavorably with all-atom normal mode analysis, the Rotation Translation Blocksprocedure, and experiment. The proposed methodology establishes a computationalframework for the calculation of protein mechanical response that facilitatesthe incorporation of specific atomic-level interactions into the model,including aqueous-electrolyte-mediated electrostatic effects. The procedure isequally applicable to proteins with known atomic coordinates as it is toelectron density maps of proteins, protein complexes, and supramolecularassemblies of unknown atomic structure.


Instruction: what is the prompt that generates the input?

Input: The conventional magnetic induction equation that governs hydromagneticdynamo action is transformed into an equivalent integral equation system. Anadvantage of this approach is that the computational domain is restricted tothe region occupied by the electrically conducting fluid and to its boundary.This integral equation approach is first employed to simulate kinematic dynamosexcited by Beltrami-like flows in a finite cylinder. The impact of externallyadded layers around the cylinder on the onset of dynamo actions isinvestigated. Then it is applied to simulate dynamo experiments withincylindrical geometry including the von Karman sodium (VKS) experiment and theRiga dynamo experiment. A modified version of this approach is utilized toinvestigate magnetic induction effects under the influence of externallyapplied magnetic fields which is also important to measure the proximity of agiven dynamo facility to the self-excitation threshold.


Instruction: what is the prompt that generates the input?

Input: We discuss in detail the problem of counting BPS gauge invariant operators inthe chiral ring of quiver gauge theories living on D-branes probing generictoric CY singularities. The computation of generating functions that includecounting of baryonic operators is based on a relation between the baryoniccharges in field theory and the Kaehler moduli of the CY singularities. A studyof the interplay between gauge theory and geometry shows that given geometricalsectors appear more than once in the field theory, leading to a notion of"multiplicities". We explain in detail how to decompose the generating functionfor one D-brane into different sectors and how to compute their relevantmultiplicities by introducing geometric and anomalous baryonic charges. ThePlethystic Exponential remains a major tool for passing from one D-brane toarbitrary number of D-branes. Explicit formulae are given for few examples,including C^3/Z_3, F_0, and dP_1.


Instruction: what is the prompt that generates the input?

Input: Onsager conjectured that weak solutions of the Euler equations forincompressible fluids in 3D conserve energy only if they have a certain minimalsmoothness, (of order of 1/3 fractional derivatives) and that they dissipateenergy if they are rougher. In this paper we prove that energy is conserved forvelocities in the function space $B^{1/3}_{3,c(\NN)}$. We show that this spaceis sharp in a natural sense. We phrase the energy spectrum in terms of theLittlewood-Paley decomposition and show that the energy flux is controlled bylocal interactions. This locality is shown to hold also for the helicity flux;moreover, every weak solution of the Euler equations that belongs to$B^{2/3}_{3,c(\NN)}$ conserves helicity. In contrast, in two dimensions, thestrong locality of the enstrophy holds only in the ultraviolet range.


Instruction: what is the prompt that generates the input?

Input: The plethora of recent cosmologically relevant data has indicated that ouruniverse is very well fit by a standard Friedmann-Lema\^{i}tre-Robertson-Walker(FLRW) model, with $\Omega_{M} \approx 0.27$ and $\Omega_{\Lambda} \approx0.73$ -- or, more generally, by nearly flat FLRW models with parameters closeto these values. Additional independent cosmological information, particularlythe maximum of the angular-diameter (observer-area) distance and the redshiftat which it occurs, would improve and confirm these results, once sufficientprecise Supernovae Ia data in the range $1.5 < z < 1.8$ become available. Weobtain characteristic FLRW closed functional forms for $C = C(z)$ and$\hat{M}_0 = \hat{M}_0(z)$, the angular-diameter distance and the density persource counted, respectively, when $\Lambda \neq 0$, analogous to those we havefor $\Lambda = 0$. More importantly, we verify that for flat FLRW models$z_{max}$ -- as is already known but rarely recognized -- the redshift of$C_{max}$, the maximum of the angular-diameter-distance, uniquely gives$\Omega_{\Lambda}$, the amount of vacuum energy in the universe, independentlyof $H_0$, the Hubble parameter. For non-flat models determination of both$z_{max}$ and $C_{max}$ gives both $\Omega_{\Lambda}$ and $\Omega_M$, theamount of matter in the universe, as long as we know $H_0$ independently.Finally, determination of $C_{max}$ automatically gives a very simpleobservational criterion for whether or not the universe is flat -- presumingthat it is FLRW.


Instruction: what is the prompt that generates the input?

Input: We introduce a simple nearest-neighbor spin model with multiple metastablephases, the number and decay pathways of which are explicitly controlled by theparameters of the system. With this model we can construct, for example, asystem which evolves through an arbitrarily long succession of metastablephases. We also construct systems in which different phases may nucleatecompetitively from a single initial phase. For such a system, we present ageneral method to extract from numerical simulations the individual nucleationrates of the nucleating phases. The results show that the Ostwald rule, whichpredicts which phase will nucleate, must be modified probabilistically when thenew phases are almost equally stable. Finally, we show that the nucleation rateof a phase depends, among other things, on the number of other phasesaccessible from it.


Instruction: what is the prompt that generates the input?

Input: We investigate the relation between thermodynamic and dynamic properties ofan associating lattice gas (ALG) model. The ALG combines a three dimensionallattice gas with particles interacting through a soft core potential andorientational degrees of freedom. From the competition between the directionalattractive forces and the soft core potential results two liquid phases, doublecriticality and density anomaly. We study the mobility of the molecules in thismodel by calculating the diffusion constant at a constant temperature, $D$. Weshow that $D$ has a maximum at a density $\rho_{max}$ and a minimum at adensity $\rho_{min}<\rho_{max}$. Between these densities the diffusivitydiffers from the one expected for normal liquids. We also show that in thepressure-temperature phase-diagram the line of extrema in diffusivity is closeto the liquid-liquid critical point and it is partially inside the temperatureof maximum density (TMD) line.


Instruction: what is the prompt that generates the input?

Input: In the present paper we study two qubit entanglement in the most general$XYZ$ Heisenberg magnetic chain with (non)homogeneous magnetic fields and theDM anisotropic antisymmetric exchange interaction, arising from the spin-orbitcoupling . The model includes all known results as particular cases, for bothantiferromagnetic and ferromagnetic $XX, XY, XXX, XXZ, XYZ$ chains. Theconcurrence of two qubit thermal entanglement and its dependence on anisotropicparameters, external magnetic field and temperature are studied in details. Wefound that in all cases, inclusion of the DM interaction, which is responsiblefor weak ferromagnetism in mainly antiferromagnetic crystals and spinarrangement in low symmetry magnets, creates (when it does not exist) orstrengthens (when it exists) entanglement in $XYZ$ spin chain. This impliesexistence of a relation between arrangement of spins and entanglement, in whichthe DM coupling plays an essential role. It suggests also that anisotropicantisymmetric exchange interaction could be an efficient control parameter ofentanglement in the general $XYZ$ case.


Instruction: what is the prompt that generates the input?

Input: We propose a new field-theoretic framework for formulating thenon-relativistic quantum mechanics of D particles in a Fock space of U(N)Yang-Mills theories with all different N in a unified way. D-particle fieldoperators, creating and annihilating a D particle and hence changing N one byone, are defined. The base space of these D-particle fields is a (complex)vector space of infinite dimensions. The gauge invariance of Yang-Mills quantummechanics is reinterpreted as a quantum-statistical symmetry, which is takeninto account by setting up a novel algebraic and projective structure in theformalism. Ordinary physical observables of Yang-Mills theory, obeying thestandard algebra, are expressed as bilinear forms of the D-particle fields.Together with the open-closed string duality, our new formulation suggests atrinity of three different but mutually dual viewpoints in string theory.


Instruction: what is the prompt that generates the input?

Input: Author offers and researches a new, cheap method for the extraction offreshwater from the Earth atmosphere. The suggected method is fundamentallydictinct from all existing methods that extract freshwater from air. All otherindustrial methods extract water from a saline water source (in most cases fromseawater). This new method may be used at any point in the Earth except PolarZones. It does not require long-distance freshwater transportation. If seawateris not utilized for increasing its productivity, this inexpensive new method isvery environment-friendly. The author method has two working versions: (1) thefirst variant the warm (hot) atmospheric air is lifted by the inflatable tubein a high altitude and atmospheric steam is condenced into freswater: (2) inthe second version, the warm air is pumped 20-30 meters under the sea-surface.In the first version, wind and solar heating of air are used for causing airflow. In version (2) wind and propeller are used for causing air movment.  The first method does not need energy, the second needs a small amount.Moreover, in variant (1) the freshwater has a high pressure (>30 or more atm.)and can be used for production of energy such as electricity and in that waythe freshwater cost is lower. For increasing the productivity the seawater isinjected into air and solar air heater may be used. The solar air heaterproduces a huge amount of electricity as a very powerful electricity generationplant. The offered electricity installation in 100 - 200 times cheaper than anycommon electric plant of equivalent output.  Key words: Extraction freshwater, method of getting freshwater, receivingenergy from atmosphere, powerful renewal electric plant.


Instruction: what is the prompt that generates the input?

Input: We present a simple implementation of the dynamical mean-field theoryapproach to the electronic structure of strongly correlated materials. Thisimplementation achieves full self-consistency over the charge density, takinginto account correlation-induced changes to the total charge density andeffective Kohn-Sham Hamiltonian. A linear muffin-tin orbital basis-set is used,and the charge density is computed from moments of the many bodymomentum-distribution matrix. The calculation of the total energy is alsoconsidered, with a proper treatment of high-frequency tails of the Green'sfunction and self-energy. The method is illustrated on two materials withwell-localized 4f electrons, insulating cerium sesquioxide Ce2O3 and thegamma-phase of metallic cerium, using the Hubbard-I approximation to thedynamical mean-field self-energy. The momentum-integrated spectral function andmomentum-resolved dispersion of the Hubbard bands are calculated, as well asthe volume-dependence of the total energy. We show that full self-consistencyover the charge density, taking into account its modification by strongcorrelations, can be important for the computation of both thermodynamical andspectral properties, particularly in the case of the oxide material.


Instruction: what is the prompt that generates the input?

Input: We consider the extent to which future imaging surveys of galaxies candistinguish between dark energy and modified gravity models for the origin ofthe cosmic acceleration. Dynamical dark energy models may have similarexpansion rates as models of modified gravity, yet predict different growth ofstructure histories. We parameterize the cosmic expansion by the twoparameters, $w_0$ and $w_a$, and the linear growth rate of density fluctuationsby Linder's $\gamma$, independently. Dark energy models generically predict$\gamma \approx 0.55$, while the DGP model $\gamma \approx 0.68$. To determineif future imaging surveys can constrain $\gamma$ within 20 percent (or$\Delta\gamma<0.1$), we perform the Fisher matrix analysis for a weak lensingsurvey such as the on-going Hyper Suprime-Cam (HSC) project. Under thecondition that the total observation time is fixed, we compute the Figure ofMerit (FoM) as a function of the exposure time $\texp$. We find that thetomography technique effectively improves the FoM, which has a broad peakaround $\texp\simeq {\rm several}\sim 10$ minutes; a shallow and wide survey ispreferred to constrain the $\gamma$ parameter. While $\Delta\gamma < 0.1$cannot be achieved by the HSC weak-lensing survey alone, one can improve theconstraints by combining with a follow-up spectroscopic survey like WFMOSand/or future CMB observations.


Instruction: what is the prompt that generates the input?

Input: The frequency distribution of DNA bases A, C, G, T exhibit fractalfluctuations ubiquitous to dynamical systems in nature. The power spectra offractal fluctuations exhibit inverse power law form signifying long-rangecorrelations between local (small-scale) and global (large-scale)perturbations. The author has developed a general systems theory based onclassical statistical physics for fractal fluctuations which predicts that theprobability distribution of eddy amplitudes and the variance (square of eddyamplitude)spectrum of fractal fluctuations follow the universal Boltzmanninverse power law expressed as a function of the golden mean. The modelpredicted distribution is very close to statistical normal distribution forfluctuations within two standard deviations from the mean and exhibits a fatlong tail. In this paper it is shown that DNA base CG frequency distribution inTakifugu rubripes (Puffer fish) Genome Release 4 exhibit universal inversepower law form consistent with model prediction. The observed long-rangecorrelations in the DNA bases implies that the non-coding 'junk' or 'selfish'DNA which appear to be redundant, may also contribute to the efficientfunctioning of the protein coding DNA, a result supported by recent studies.


Instruction: what is the prompt that generates the input?

Input: We consider power allocation algorithms for fixed-rate transmission overNakagami-m non-ergodic block-fading channels with perfect transmitter andreceiver channel state information and discrete input signal constellationsunder both short- and long-term power constraints. Optimal power allocationschemes are shown to be direct applications of previous results in theliterature. We show that the SNR exponent of the optimal short-term scheme isgiven by the Singleton bound. We also illustrate the significant gainsavailable by employing long-term power constraints. Due to the nature of theexpressions involved, the complexity of optimal schemes may be prohibitive forsystem implementation. We propose simple sub-optimal power allocation schemeswhose outage probability performance is very close to the minimum outageprobability obtained by optimal schemes.


Instruction: what is the prompt that generates the input?

Input: I show that several observable properties of bursting neutron stars in metrictheories of gravity can be calculated using only conservation laws, Killingsymmetries, and the Einstein equivalence principle, without requiring thevalidity of the general relativistic field equations. I calculate, inparticular, the gravitational redshift of a surface atomic line, the touchdownluminosity of a radius-expansion burst, which is believed to be equal to theEddington critical luminosity, and the apparent surface area of a neutron staras measured during the cooling tails of bursts. I show that, for a generalmetric theory of gravity, the apparent surface area of a neutron star dependson the coordinate radius of the stellar surface and on its gravitationalredshift in the exact same way as in general relativity. On the other hand, theEddington critical luminosity depends also on an additional parameter thatmeasures the degree to which the general relativistic field equations aresatisfied. These results can be used in conjunction with current and futurehigh-energy observations of bursting neutron stars to test general relativityin the strong-field regime.


Instruction: what is the prompt that generates the input?

Input: The MuCap experiment is a high-precision measurement of the rate for thebasic electroweak process of muon capture, mu- + p -> n + nu . The experimentalapproach is based on an active target consisting of a time projection chamber(TPC) operating with pure hydrogen gas. The hydrogen has to be kept extremelypure and at a stable pressure. A Circulating Hydrogen Ultrahigh PurificationSystem was designed at the Petersburg Nuclear Physics Institute (PNPI) tocontinuously clean the hydrogen from impurities. The system is based on anadsorption cryopump to stimulate the hydrogen flow and on a cold adsorbent forthe hydrogen cleaning. It was installed at the Paul Scherrer Institute (PSI) in2004 and performed reliably during three experiment runs. During several monthslong operating periods the system maintained the hydrogen purity in thedetector on the level of 20 ppb for moisture, which is the main contaminant,and of better than 7 ppb and 5 ppb for nitrogen and oxygen, respectively. Thepressure inside the TPC was stabilized to within 0.024% of 10 bar at a hydrogenflow rate of 3 standard liters per minute.


Instruction: what is the prompt that generates the input?

Input: The classical Euler's problem on stationary configurations of elastic rodwith fixed endpoints and tangents at the endpoints is considered as aleft-invariant optimal control problem on the group of motions of atwo-dimensional plane $\E(2)$.  The attainable set is described, existence and boundedness of optimalcontrols are proved. Extremals are parametrized by Jacobi's elliptic functionsof natural coordinates induced by the flow of the mathematical pendulum onfibers of the cotangent bundle of $\E(2)$.  The group of discrete symmetries of Euler's problem generated by reflectionsin the phase space of the pendulum is studied. The corresponding Maxwell pointsare completely described via the study of fixed points of this group. As aconsequence, an upper bound on cut points in Euler's problem is obtained.


Instruction: what is the prompt that generates the input?

Input: We present here a detailed study of the behaviour of a three dimensionalBrownian motor based on cold atoms in a double optical lattice [P. Sjolund etal., Phys. Rev. Lett. 96, 190602 (2006)]. This includes both experiments andnumerical simulations of a Brownian particle. The potentials used are spatiallyand temporally symmetric, but combined spatiotemporal symmetry is broken byphase shifts and asymmetric transfer rates between potentials. The diffusion ofatoms in the optical lattices is rectified and controlled both in direction andspeed along three dimensions. We explore a large range of experimentalparameters, where irradiances and detunings of the optical lattice lights arevaried within the dissipative regime. Induced drift velocities in the order ofone atomic recoil velocity have been achieved.


Instruction: what is the prompt that generates the input?

Input: An automated magnetometer suitable for long lasting measurement under stableand controllable experimental conditions has been implemented. The device isbased on Coherent Population Trapping (CPT) produced by a multi-frequencyexcitation. CPT resonance is observed when a frequency comb, generated by diodelaser current modulation, excites Cs atoms confined in a$\pi/4\times(2.5)^2\times1 \textrm{cm}^3$, 2 Torr $N_2$ buffered cell. A fullyoptical sensor is connected through an optical fiber to the laser head allowingfor truly remote sensing and minimization of the field perturbation. A detailedanalysis of the CPT resonance parameters as a function of the optical detuninghas been made in order to get high sensitivity measurements. The magnetic fieldmonitoring performances and the best sensitivity obtained in a balanceddifferential configuration of the sensor are presented.


Instruction: what is the prompt that generates the input?

Input: Plasmas in an accretion flow are heated by MHD turbulence generated throughthe magneto-rotational instability. The viscous stress driving the accretion isintimately connected to the microscopic processes of turbulence dissipation. Weshow that, in a few well-observed black hole accretion systems, there iscompelling observational evidence of efficient electron heating by turbulenceor collective plasma effects in low accretion states, when Coulomb collisionsare not efficient enough to establish a thermal equilibrium between electronsand ions at small radii. However, charged particles reach a thermal equilibriumwith their kind much faster than with others through Coulomb collisions, atwo-temperature accretion flow is expected. We consider a Keplerian accretionflow with a constant mass accretion rate in the pseudo-Newtonian gravitationalpotential and take into account the bremsstrahlung, synchrotron, and inverseComptonization cooling processes. The critical mass accretion rate, below whichthe two-temperature solution may exist, is determined by the cooling processesand the collisional energy exchanges between electrons and ions and has veryweak dependence on the collision-less heating of electrons by turbulence, whichbecomes more important at lower accretion rates. Collision-less heating ofelectrons by MHD turbulence can no longer be ignored in quantitativeinvestigations of these systems.


Instruction: what is the prompt that generates the input?

Input: We consider a three dimensional system consisting of a large number of smallspherical particles, distributed in a range of sizes and heights (with uniformdistribution in the horizontal direction). Particles move vertically at asize-dependent terminal velocity. They are either allowed to merge wheneverthey cross or there is a size ratio criterion enforced to account for collisionefficiency. Such a system may be described, in mean field approximation, by theSmoluchowski kinetic equation with a differential sedimentation kernel, used tostudy e.g. rain initiation and particle distributions in the atmosphere. Wesolve the kinetic equation analytically to obtain steady state and self-similarsolutions in time and in height, using methods borrowed from weak turbulencetheory. Analytical results are compared with direct numerical simulations (DNS)of moving and merging particles, and a good agreement is found.


Instruction: what is the prompt that generates the input?

Input: We consider anisotropic magnetized cosmologies filled with conductive plasmafluid and study the implications of metric perturbations that propagateparallel to the ambient magnetic field. It is known that in the first order(linear) approximation with respect to the amplitude of the perturbations noelectric field and density perturbations arise. However, when we consider thenon-linear coupling of the metric perturbations with their temporalderivatives, certain classes of solutions can induce steeply increasing in timeelectric field perturbations. This is verified both numerically andanalytically. The source of these perturbations can be either high-frequencyquantum vacuum fluctuations, driven by the cosmological pump field, in theearly stages of the evolution of the Universe or astrophysical processes or anon-linear isotropization process of an initially anisotropic cosmologicalspacetime.


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Input: An extensive literature exists describing various techniques for theevaluation of Hankel determinants. The prevailing methods such as Dodgsoncondensation, continued fraction expansion, LU decomposition, all produceproduct formulas when they are applicable. We mention the classic case of theHankel determinants with binomial entries ${3k+2 \choose k}$ and those withentries ${3k \choose k}$; both of these classes of Hankel determinants haveproduct form evaluations. The intermediate case, ${3k+1 \choose k}$ has notbeen evaluated. There is a good reason for this: these latter determinants donot have product form evaluations.  In this paper we evaluate the Hankel determinant of ${3k+1 \choose k}$. Theevaluation is a sum of a small number of products, an almost product.  The method actually provides more, and as applications, we present thesalient points for the evaluation of a number of other Hankel determinants withpolynomial entries, along with product and almost product form evaluations atspecial points.


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Input: A new catalogue of extended radio sources has been prepared based onarcminute-resolution 1420 MHz images from the Canadian Galactic Plane Survey(CGPS). The new catalogue provides both 1420 MHz and 408 MHz flux densitymeasurements on sources found near the Galactic plane in the second quadrant ofour Galaxy. In addition cross-identifications are made with other major radiocatalogues and information is provided to facilitate the recovery of CGPS imagedata associated with each catalogued source. Numerous new radio sources areidentified and the catalogue provides a comprehensive summary of both newlydiscovered and previously known HII regions and supernova remnants in the outerGalaxy. The catalogue should be of use both for synoptic studies of Galacticstructure and for placing higher resolution observations, at radio and otherwavelengths, in context.


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Input: We have investigated the possibility of direct tests of little Higgs modelsincorporating triplet Higgs neutrino mass mechanism at LHC experiments. We haveperformed Monte Carlo studies of Drell-Yan pair production of doubly chargedHiggs boson \Phi^{++} followed by its leptonic decays which branching ratiosare fixed from the neutrino oscillation data. We propose appropriate selectionrules for the four-lepton signal, including reconstructed taus, which areoptimized for the discovery of \Phi^{++} with the lowest LHC luminosity. As theStandard Model background can be effectively eliminated, an important aspect ofour study is the correct statistical treatment of the LHC discovery potential.Adding detection efficiencies and measurement errors to the Monte Carloanalyses, \Phi^{++} can be discovered up to the mass 250 GeV in the first yearof LHC, and 700 GeV mass is reachable for the integrated luminosity L=30fb^{-1}.


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Input: A new class of Erbium doped glasses with compositions xNa2O - (60-x)PbCl2 -40P2O5 (x=0, 10, 20 and 30) were fabricated and characterized for opticalproperties. Absorption spectra were analyzed for important Judd-Ofeltparameters from the integrated intensities of various Er3+ glass absorptionbands. Photoluminescence (PL) and its decay behavior studies were carried outfor the transition 4I13/2 -> 4I15/2. A systematic correlation between theJudd-Ofelt parameter {omega}2 and the covalent nature of the glass matrix wasobserved, due to increased role of bridging oxygens in the glass network. ThePL broadness and life times of 4I13/2_> 4I15/2 transition were typically in therange of 40-60nm and 2.13-2.5ms respectively. These glasses broadly showed hightransparency, high refractive index, shorter life times and, most importantly,these glasses were found to be capable of being doped with largerconcentrations of Er3+ (up to 4 wt%). Increase of Er3+ concentration resultedin the increase in PL line-widths with no significant effect of concentrationquenching, indicating that these glasses are suitable for opticalfibre/waveguide amplifiers.


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Input: We consider the interpretation of tetrad fields as reference frames inspacetime. Reference frames may be characterized by an antisymmetricacceleration tensor, whose components are identified as the inertialaccelerations of the frame (the translational acceleration and the frequency ofrotation of the frame). This tensor is closely related togravitoelectromagnetic field quantities. We construct the set of tetrad fieldsadapted to observers that are in free fall in the Schwarzschild spacetime, andshow that the gravitational energy-momentum constructed out of this set oftetrad fields, in the framework of the teleparallel equivalent of generalrelatrivity, vanishes. This result is in agreement with the principle ofequivalence, and may be taken as a condition for a viable definition ofgravitational energy.


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Input: The following question is addressed: under what conditions can a strangediffusive process, defined by a semi-dynamical V-Langevin equation or itsassociated Hybrid kinetic equation (HKE), be described by an equivalent purelystochastic process, defined by a Continuous Time Random Walk (CTRW) or by aFractional Differential Equation (FDE)? More specifically, does there exist aclass of V-Langevin equations with long-range (algebraic) velocity temporalcorrelation, that leads to a time-fractional superdiffusive process? The answeris always affirmative in one dimension. It is always negative in twodimensions: any algebraically decaying temporal velocity correlation (with aGaussian spatial correlation) produces a normal diffusive process. Generalconditions relating the diffusive nature of the process to the temporalexponent of the Lagrangian velocity correlation (in Corrsin approximation) arederived.


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Input: This is a sequel to [Ca01]=math.AG/0110051. We define the bimeromorphic {\itcategory} of geometric orbifolds. These interpolate between (compact K\" ahler)manifolds and such manifolds with logarithmic structure. These geometricorbifolds are considered from the point of view of their geometry, and thusequipped with the usual invariants of varieties: morphisms and bimeromorphicmaps, differential forms, fundamental groups and universal covers, fields ofdefinition and rational points. The most elementary properties, directlyadapted from the case of varieties without orbifold structure, are establishedhere. The arguments of [Ca01] can then be directly adapted to extend the mainstructure results to this orbifold category. We hope to come back to deeperaspects later. The motivation is that the natural frame for the theory ofclassification of compact K\" ahler (and complex projective) manifolds includesat least the category of orbifolds, as shown in [Ca01] by the fonctorialdecomposition of {\it special} manifolds as tower of orbifolds with either$\kappa_+=-\infty$ or $\kappa=0$, and also, seemingly, by the minimal modelprogram, in which most proofs work only after the adjunction of a "boundary".  Also, fibrations enjoy in the bimeromorphic category of geometric orbifoldsextension properties not satisfied in the category of varieties withoutorbifold structure, permitting to express invariants of the total space fromthose of the generic fibre and of the base. For example, the natural sequenceof fundamental groups is exact there; also the total space is special if so arethe generic fibre and the base. This makes this category suitable to liftproperties from orbifolds having either $\kappa_+=-\infty$ or $\kappa=0$ tothose which are special.


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Input: Current methods for producing single-walled carbon nanotubes (SWNTs) lead toheterogeneous samples containing mixtures of metallic and semiconductingspecies with a variety of lengths and defects. Optical detection at the singlenanotube level should thus offer the possibility to examine theseheterogeneities provided that both SWNT species are equally well detected.Here, we used photothermal heterodyne detection to record absorption images andspectra of individual SWNTs. Because this photothermal method relies only onlight absorption, it readily detects metallic nanotubes as well as the emissivesemiconducting species. The first and second optical transitions in individualsemicontucting nanotubes have been probed. Comparison between the emission andabsorption spectra of the lowest-lying optical transition reveal mainly smallStokes shifts. Side bands in the near-infrared absorption spectra are observedand assigned to exciton-phonon bound states. No such sidebands are detectedaround the lowest transition of metallic nanotubes.


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Input: Max-product belief propagation is a local, iterative algorithm to find themode/MAP estimate of a probability distribution. While it has been successfullyemployed in a wide variety of applications, there are relatively fewtheoretical guarantees of convergence and correctness for general loopy graphsthat may have many short cycles. Of these, even fewer provide exact ``necessaryand sufficient'' characterizations.  In this paper we investigate the problem of using max-product to find themaximum weight matching in an arbitrary graph with edge weights. This is doneby first constructing a probability distribution whose mode corresponds to theoptimal matching, and then running max-product. Weighted matching can also beposed as an integer program, for which there is an LP relaxation. Thisrelaxation is not always tight. In this paper we show that \begin{enumerate}\item If the LP relaxation is tight, then max-product always converges, andthat too to the correct answer. \item If the LP relaxation is loose, thenmax-product does not converge. \end{enumerate} This provides an exact,data-dependent characterization of max-product performance, and a preciseconnection to LP relaxation, which is a well-studied optimization technique.Also, since LP relaxation is known to be tight for bipartite graphs, ourresults generalize other recent results on using max-product to find weightedmatchings in bipartite graphs.


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Input: We consider the discretization  y(t+\epsilon)=y(t-\epsilon)+2\epsilon\big(1-y(t)^{2}\big),  $\epsilon>0$ a small parameter, of the logistic differential equation$y'=2\big(1-y^{2}\big)$, which can also be seen as a discretization of thesystem  {y'=2\big(1-v^{2}\big),  v'= 2\big(1-y^{2}\big).  This system has two saddle points at $A=(1,1)$, $B=(-1, -1)$ and there existstable and unstable manifolds. We will show that the stable manifold$W_{s}^{+}$ of the point $A=(1,1)$ and the unstable manifold $W_{i}^{-}$ of thepoint $B=(-1, -1)$ for the discretization do not coincide. The verticaldistance between these two manifolds is exponentially small but not zero, inparticular we give an asymptotic estimate of this distance. For this purpose wewill use a method adapted from the paper of Sch\"afke-Volkmer \cite{SV} usingformal series and accurate estimates of the coefficients.


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Input: This paper follows in the tradition of direct-action versions ofelectromagnetism having the aim of avoiding a balance of infinities wherein amechanical mass offsets an infinite electromagnetic mass so as to arrive at afinite observed value. Given that, in this respect the direct-action approachedultimately failed because its initial exclusion of self-action was found to beuntenable in the relativistic domain, this paper continues the traditionconsidering instead a version of electromagnetism wherein mechanical action isexcluded and self-action is retained. It is shown that the resulting theory iseffectively interacting due to the presence of infinite forces. A vehicle forthe investigation is a pair of classical point charges in a positronium-likearrangement for which the orbits are found to be self-sustaining and naturallyquantized.


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Input: Annealed importance sampling is a means to assign equilibrium weights to anonequilibrium sample that was generated by a simulated annealing protocol. Theweights may then be used to calculate equilibrium averages, and also serve asan ``adiabatic signature'' of the chosen cooling schedule. In this paper wedemonstrate the method on the 50-atom dileucine peptide, showing thatequilibrium distributions are attained for manageable cooling schedules. Forthis system, as naively implemented here, the method is modestly more efficientthan constant temperature simulation. However, the method is worth consideringwhenever any simulated heating or cooling is performed (as is often done at thebeginning of a simulation project, or during an NMR structure calculation), asit is simple to implement and requires minimal additional CPU expense.Furthermore, the naive implementation presented here can be improved.


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Input: Random walks on expander graphs were thoroughly studied, with the importantmotivation that, under some natural conditions, these walks mix quickly andprovide an efficient method of sampling the vertices of a graph. Alon,Benjamini, Lubetzky and Sodin studied non-backtracking random walks on regulargraphs, and showed that their mixing rate may be up to twice as fast as that ofthe simple random walk. As an application, they showed that the maximal numberof visits to a vertex, made by a non-backtracking random walk of length $n$ ona high-girth $n$-vertex regular expander, is typically $(1+o(1))\frac{\logn}{\log\log n}$, as in the case of the balls and bins experiment. They furtherasked whether one can establish the precise distribution of the visits such awalk makes.  In this work, we answer the above question by combining a generalized form ofBrun's sieve with some extensions of the ideas in Alon et al. Let $N_t$ denotethe number of vertices visited precisely $t$ times by a non-backtracking randomwalk of length $n$ on a regular $n$-vertex expander of fixed degree and girth$g$. We prove that if $g=\omega(1)$, then for any fixed $t$, $N_t/n$ istypically $\frac{1}{\mathrm{e}t!}+o(1)$. Furthermore, if $g=\Omega(\log\logn)$, then $N_t/n$ is typically $\frac{1+o(1)}{\mathrm{e}t!}$ uniformly on all$t \leq (1-o(1))\frac{\log n}{\log\log n}$ and 0 for all $t \geq(1+o(1))\frac{\log n}{\log\log n}$. In particular, we obtain the above resulton the typical maximal number of visits to a single vertex, with an improvedthreshold window. The essence of the proof lies in showing that variablescounting the number of visits to a set of sufficiently distant vertices areasymptotically independent Poisson variables.


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Input: The photon box thought experiment can be considered a forerunner of theEPR-experiment: by performing suitable measurements on the box it is possibleto ``prepare'' the photon, long after it has escaped, in either of twocomplementary states. Consistency requires that the corresponding boxmeasurements be complementary as well. At first sight it seems, however, thatthese measurements can be jointly performed with arbitrary precision: theypertain to different systems (the center of mass of the box and an internalclock, respectively). But this is deceptive. As we show by explicitcalculation, although the relevant quantities are simultaneously measurable,they develop non-vanishing commutators when calculated back to the time ofescape of the photon. This justifies Bohr's qualitative arguments in a preciseway; and it illustrates how the details of the dynamics conspire to guaranteethe requirements of complementarity. In addition, our calculations exhibit a``fine structure'' in the distribution of the uncertainties over thecomplementary quantities: depending on when the box measurement is performed,the resulting quantum description of the photon differs. This brings us closeto the argumentation of the later EPR thought experiment.


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Input: Density-functional theory requires ever better exchange-correlation (xc)functionals for the ever more precise description of many-body effects onelectronic structure. Universal constraints on the xc energy are importantingredients in the construction of improved functionals. Here we investigateone such universal property of xc functionals: the Lieb-Oxford lower bound onthe exchange-correlation energy, $E_{xc}[n] \ge -C \int d^3r n^{4/3}$, where$C\leq C_{LO}=1.68$. To this end, we perform a survey of available exact ornear-exact data on xc energies of atoms, ions, molecules, solids, and somemodel Hamiltonians (the electron liquid, Hooke's atom and the Hubbard model).All physically realistic density distributions investigated are consistent withthe tighter limit $C \leq 1$. For large classes of systems one can obtainclass-specific (but not fully universal) similar bounds. The Lieb-Oxford boundwith $C_{LO}=1.68$ is a key ingredient in the construction of modern xcfunctionals, and a substantial change in the prefactor $C$ will haveconsequences for the performance of these functionals.


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Input: The aim of the present paper is to provide a global presentation of thetheory of special Finsler manifolds. We introduce and investigate globally (orintrinsically, free from local coordinates) many of the most important and mostcommonly used special Finsler manifolds: locally Minkowskian, Berwald,Landesberg, general Landesberg, $P$-reducible, $C$-reducible,semi-$C$-reducible, quasi-$C$-reducible, $P^{*}$-Finsler, $C^{h}$-recurrent,$C^{v}$-recurrent, $C^{0}$-recurrent, $S^{v}$-recurrent, $S^{v}$-recurrent ofthe second order, $C_{2}$-like, $S_{3}$-like, $S_{4}$-like, $P_{2}$-like,$R_{3}$-like, $P$-symmetric, $h$-isotropic, of scalar curvature, of constantcurvature, of $p$-scalar curvature, of $s$-$ps$-curvature. The globaldefinitions of these special Finsler manifolds are introduced. Variousrelationships between the different types of the considered special Finslermanifolds are found. Many local results, known in the literature, are provedglobally and several new results are obtained. As a by-product, interestingidentities and properties concerning the torsion tensor fields and thecurvature tensor fields are deduced. Although our investigation is entirelyglobal, we provide; for comparison reasons, an appendix presenting a localcounterpart of our global approach and the local definitions of the specialFinsler spaces considered.


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Input: By combining the local density approximation (LDA) with dynamical mean fieldtheory (DMFT), we report a systematic analysis of the spectral properties of$\delta$-plutonium with varying $5f$ occupancy. The LDA Hamiltonian isextracted from a tight-binding (TB) fit to full-potential linearized augmentedplane-wave (FP-LAPW) calculations. The DMFT equations are solved by the exactquantum Monte Carlo (QMC) method and the Hubbard-I approximation. We have shownfor the first time the strong sensitivity of the spectral properties to the$5f$ occupancy, which suggests using this occupancy as a fitting parameter inaddition to the Hubbard $U$. By comparing with PES data, we conclude that the``open shell'' $5f^{5}$ configuration gives the best agreement, resolving thecontroversy over $5f$ ``open shell'' versus ``close shell'' atomicconfigurations in $\delta$-Pu.


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Input: The extraction of the weak phase $\alpha$ from $B\to\pi\pi$ decays has beencontroversial from a statistical point of view, as the frequentist vs. bayesianconfrontation shows. We analyse several relevant questions which have notdeserved full attention and pervade the extraction of $\alpha$.Reparametrization Invariance proves appropriate to understand those issues. Weshow that some Standard Model inspired parametrizations can be senseless orinadequate if they go beyond the minimal Gronau and London assumptions: thesingle weak phase $\alpha$ just in the $\Delta I=3/2$ amplitudes, the isospinrelations and experimental data. Beside those analyses, we extract $\alpha$through the use of several adequate parametrizations, showing that there is norelevant discrepancy between frequentist and bayesian results. The mostrelevant information, in terms of $\alpha$, is the exclusion of values around$\alpha\sim \pi/4$; this result is valid in the presence of arbitrary NewPhysics contributions to the $\Delta I=1/2$ piece.


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Input: We present observations of the (1,1), (2,2), (4,4) and (5,5) inversiontransitions of para-ammonia (NH3) and 24 GHz continuum, taken with theAustralia Telescope Compact Array toward 21 southern Galactic hot molecularcores traced by 6.7 GHz methanol maser emission. We detect NH3(1,1) emissiontoward all 21 regions and 24 GHz continuum emission toward 12 of the regions,including 6 with no reported 8 GHz continuum counterparts. In total, we findthe 21 regions contain 41 NH3(1,1) cores. We extract characteristic spectra forevery core at each of the NH3 transitions and present both integrated intensitymaps and channel maps for each region. The NH3(4,4)+(5,5) emission is alwaysunresolved and found at the maser position indicating that the methanol masersare found at the warmest part of the core. We observe large asymmetries in theNH3(1,1) hyperfine line profiles and conclude this is due to a number of dense,small clumps within the beam. We derive properties of the ionised gas and findthe 24 GHz continuum sources not detected at 8 GHz are always coincident withboth NH3 and methanol masers in contrast to those detected at 8 + 24 GHz whichare generally offset from the methanol masers. We investigate the possibilitythat the former may be hyper-compact HII regions. Finally, we separate thecores into five groups, based on their association with NH3, methanol maser andcontinuum emission. From the different physical properties of the cores in thegroups, we discuss the possibility that these groups may represent cores atdifferent evolutionary stages of the massive star formation process.


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Input: A discrete tensegrity framework can be thought of as a graph in Euclideann-space where each edge is of one of three types: an edge with a fixed length(bar) or an edge with an upper (cable) or lower (strut) bound on its length.Roth and Whiteley, in their 1981 paper "Tensegrity Frameworks", showed that incertain cases, the struts and cables can be replaced with bars when analyzingthe framework for infinitesimal rigidity. In that case we call the tensegrity"bar equivalent". In specific, they showed that if there exists a set ofpositive weights, called a positive "stress", on the edges such that theweighted sum of the edge vectors is zero at every vertex, then the tensegrityis bar equivalent.  In this paper we consider an extended version of the tensegrity framework inwhich the vertex set is a (possibly infinite) set of points in Euclideann-space and the edgeset is a compact set of unordered pairs of vertices. Theseare called "continuous tensegrities". We show that if a continuous tensegrityhas a strictly positive stress, it is bar equivalent and that it has asemipositive stress if and only if it is partially bar equivalent. We also showthat if a tensegrity is minimally bar equivalent (it is bar equivalent butremoving any open set of edges makes it no longer so), then it has a strictlypositive stress.  In particular, we examine the case where the vertices form a rectifiablecurve and the possible motions of the curve are limited to local isometries ofit. Our methods provide an attractive proof of the following result: There isno locally arclength preserving motion of a circle that increases any antipodaldistance without decreasing some other one.


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Input: In this paper, we investigate a new waveform for UWB systems obtained by thecombination of Orthogonal Frequency Division Multiplex (OFDM) and Code DivisionMultiple Access (CDMA). The proposed system, called Spread Spectrum -Multi-Carrier - Multiple Access (SS-MC-MA) turns out to be a judicious solutionto combat frequency selectivity and narrowband interferers, and to manage thecoexistence of several users and piconets. It is shown that the addition of adegree of freedom brought by the spreading component of SS-MC-MA allows tooptimize jointly the assignment of the number of used codes and coding rates inorder to make the system more robust. Through simulations, it is demonstratedthat the new system can outperform Multi-Band OFDM Alliance (MBOA) for low datarates and is able to provide wider range of rates.


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Input: For many years various asymmetrical profiles of different spectral linesemitted from solar flares have been frequently observed. These asymmetries orline shifts are caused predominantly by vertical mass motions in flaring layersand they provide a good diagnostics for plasma flows during solar flares. Thereare many controversial results of observations and theoretical analysis ofplasma flows in solar chromospheric flares. The main difficulty is theinterpretation of line shifts or asymmetries. For many years, methods based onbisector techniques were used but they give a reliable results only for somespecific conditions and in most cases cannot be applied. The most promisingapproach is to use the non-LTE techniques applied for flaring atmosphere. Thecalculation of synthetic line profiles is performed with the radiative transfertechniques and the assumed physical conditions correspond to flaringatmosphere. I will present an overview of different observations andinterpretations of line asymmetries in chromospheric flares. I will explainwhat we have learnt about the chromospheric evaporation in the frame ofhydrodynamical models as well as reconnection models. A critical review will bedone on the classical methods used to derive Doppler-shifts for optically thickchomospheric lines. In particular, details on the new approach for interpretingchromospheric line asymmetries based on the non-LTE techniques will bepresented.