Luminous Parts Research Articles

RESOURCE-SAVING ORGANIZATIONAL AND TECHNOLOGICAL LIGHTING SOLUTIONS FOR HOUSING AND COMMUNAL SERVICES

At the turn of the two millennium, the fundamental difference in assessing the goals and means of scientific and technological progress is the consideration of architectural and planning decisions, technical and economic parameters and environmental consequences. The global nature of human impact on the habitat determines the strict requirements for choosing the parameters for the implementation of technological solutions, in particular light solutions for housing and communal services. The dynamics of electricity consumption and heat resources in Russia as a whole, including the population, was considered. The reasons for the loss of energy resources from the positions of various authors, including theft, illegal tie-ins, damage in distribution networks, insufficient level of advertising of technical and organizational and managerial innovations, are summarized. Systematized lighting solutions patented over the past 5 years in Russia, including building blocks with suspensions, hybrid lamps, heat flux sensors, luminous building parts. It was revealed that many innovative developments are based on LED solutions. The level of normative natural and cost expenditures of resources for collections of state elementary norms and federal unit rates for the construction of walls and partitions made of glass blocks was analyzed. The use of LED lighting for housing and communal services is justified. It was concluded that the power consumption when using LED lamps is several times lower than incandescent lamps and fluorescent lamps.

Dynamics and shocks from H α emission of nearby galaxy mergers

We examine the dynamical properties of interacting galaxies and the properties of shocked gas produced as a result of the interaction. We observed 22 galaxy mergers using the SparsePak IFU at Kitt Peak National Observatory (KPNO). The goal of the observations was to obtain the \ha\ velocity maps over the entire luminous parts of the galaxies including the faint tidal tails and to find extended shocks and outflows. Our sample consists of major and minor galaxy mergers with mass ratios $1<\mu<8$. We fit multiple kinematic components to the \ha\ and \nii\ emission lines, develop an MCMC code to robustly estimate the error of fit parameters, and use the F-test to determine the best number of kinematic components for each fiber. We use \nii/\ha\ and velocity dispersion of components to separate star-forming (HII) regions from shocks. We use the kinematics of the \ha\ emission from HII regions and an automated modeling method to put the first-ever constraints on the encounter parameters of one of the observed systems. Besides, we roughly estimate the fraction of shocked \ha\ emission , $\text{f}_\text{shocked}$, without taking extinction into account and examine the spatial distribution of shocks. We find that close galaxy pairs have, on average, a higher shock fraction than wide pairs, and coalesced mergers have the highest average $\text{f}_\text{shocked}$. In addition, galaxy pairs with more equal mass ratio tend to have a higher $\text{f}_\text{shocked}$. Combining the dynamical models from the literature and this work, we inspect trends between $\text{f}_\text{shocked}$ and dynamical encounter parameters. Our findings are generally consistent with shocks being produced either by the direct collision of the ISM or by the chain of events provoked by the tidal impulse during the first passage.

Analysis of UGR Values and Results of UGR Calculations in Commercial Lighting Simulation Software

ABSTRACTThe Unified Glare Rating (UGR) is an international index presented by the CIE that quantifies discomfort glare and has become of recent important. The UGR can be calculated using commercial lighting simulation software such as Relux 2013, AGi32 v2.04, and Dialux 4.11, but the values vary depending on which software is used. It appears that because the UGR input variables used in the UGR calculations of commercial lighting simulation software differ, there are differences in the calculated UGR values. Therefore, this study modified the UGR calculation modeling and made it possible to calculate UGR values with various calculation conditions of input variables. Then, the UGR values were calculated by changing calculation conditions under the following three input variables: field of view for the calculation of the background luminance (Lb) and for the calculation of luminance of the luminous parts of each luminaire (L) and the position index (P). Among the calculation conditions under these three input variables, the conditions that have an effect on the UGR values have been analyzed, and these UGR values were compared to those from commercial lighting simulation software, from which we could speculate the UGR calculation algorithm in commercial lighting simulation.

The Design of Jacquard Fabric with Optical Fiber for Effect of Leaves Falling

The optical jacquard decorative fabric which had patterns in dynamic display was woven with side-emitting polymer optical fibers (POF) and common textile fibers. The side-emitting POFs were designed as surface wefts in luminous parts of the fabric, and the POFs were back in other parts. These POFs were divided into different groups according to luminous sequence. Then the POFs were connected with light sources and a specific circuit. Finally the patterns of fabric could display like animation. When POFs didnt emit light, the fabric kept the effect of traditional jacquard fabric.

Probing non-spherical dark halos in the Galactic dwarf satellites

AbstractWe construct axisymmetric mass models for dwarf spheroidal (dSph) galaxies in the Milky Way to obtain realistic limits on the non-spherical structure of their dark halos. This is motivated by the fact that the observed luminous parts of the dSphs are actually non-spherical and cold dark matter models predict non-spherical virialized dark halos on sub-galactic scales. Applying these models to line-of-sight velocity dispersion profiles along three position angles in six Galactic satellites, we find that the best fitting cases for most of the dSphs yield not spherical but oblate and flattened dark halos. We also find that the mass of the dSphs enclosed within inner 300 pc varies depending on their total luminosities, contrary to the conclusion of previous spherical models. This suggests the importance of considering non-spherical shapes of dark halos in dSph mass models.

The large-scale cross-correlation of Damped Lyman alpha systems with the Lyman alpha forest: first measurements from BOSS

We present the first measurement of the large-scale cross-correlation of Lyα forest absorption and Damped Lyman α systems (DLA),using the 9th Data Release of the Baryon Oscillation Spectroscopic Survey (BOSS). The cross-correlation is clearlydetected on scales up to 40h−1Mpc and is well fittedby the linear theory prediction of the standard Cold Dark Matter modelof structure formation with the expected redshift distortions,confirming its origin in the gravitational evolution of structure.The amplitude of the DLA-Lyα cross-correlation depends on only one freeparameter, the bias factor of the DLA systems, once the Lyα forest biasfactors are known from independent Lyα forest correlation measurements.We measure the DLA bias factor to be bD = (2.17±0.20)βF0.22, where the Lyα forest redshift distortion parameterβF is expected to be above unity. This bias factor implies atypical host halo mass for DLAs that is much larger than expected inpresent DLA models, and is reproduced if the DLA cross section scaleswith halo mass as Mhα, with α = 1.1±0.1 forβF = 1. Matching the observed DLA bias factor and rate of incidencerequires that atomic gas remains extended in massive halos over largerareas than predicted in present simulations of galaxy formation, withtypical DLA proper sizes larger than 20 kpc in host halos of masses ∼ 1012M☉. We infer that typical galaxies at z ≃ 2 to3 are surrounded by systems of atomic clouds that are much more extendedthan the luminous parts of galaxies and contain ∼ 10% of thebaryons in the host halo.

PROBING NON-SPHERICAL DARK HALOS IN THE GALACTIC DWARF GALAXIES

We construct axisymmetric mass models for dwarf spheroidal (dSph) galaxies in the Milky Way to obtain plausible limits on the non-spherical structure of their dark halos. This is motivated by the fact that the observed luminous parts of the dSphs are actually non-spherical and Cold Dark Matter (CDM) models predict non-spherical virialized dark halos. Our models consider velocity anisotropy of stars $\bar{v^2_R} / \bar{v^2_{\phi}}$, which can vary with the adopted cylindrical coordinates under the assumption $\bar{v^2_z}=\bar{v^2_R}$ for simplicity, and also include an inclination of the system as a fitting parameter to explain the observed line-of-sight velocity dispersion profile. Applying these models to six of the bright dSphs in the Milky Way, we find that the best-fitting cases for most of the dSphs yield oblate and flattened dark halos, irrespective of assumed density profiles in their central parts. We also find that the total mass of the dSphs enclosed within a spheroid with major-axis length of 300 pc varies from $10^6M_{\odot}$ to $10^7M_{\odot}$, contrary to the conclusion from spherical models. This suggests the importance of considering shapes of dark halos in mass models of the dSphs. It is also found that dark halos of the Galactic dSphs may be more flattened than N-body predictions, thereby implying our yet incomplete understanding of baryonic and/or non-baryonic dark matter physics in dwarf galaxy scales.

ASwiftGaze into the 2006 March 29 Burst Forest of SGR 1900+14

In 2006 March the soft gamma-ray repeater SGR 1900+14 resumed its bursting activity after ~2 yr of quiescence. The Swift mission observed the source several times. We report on the intense burst forest recorded on March 29, which lasted for ~30 s, when Swift was pointing at the source with the narrow field of view instruments. More than 40 bursts were detected by BAT and XRT, 7 of which were rare intermediate flares (IFs). The BAT data were used to carry out time-resolved spectroscopy in the 14-100 keV range down to 8 ms timescales. BAT and XRT simultaneous data were used to characterize the broadband energy spectra of IFs and verify the results obtained from the BAT-only spectral fits. This unique data set allowed us to test the magnetar model predictions, such as the magnetically trapped fireball and twisted magnetosphere, over an unprecedented range of fluxes and with large statistics. We confirmed that a two-blackbody component adequately fits the time-resolved and integrated spectra of IFs. However, Comptonization models give comparably good reduced χ2. Moreover, we found a change of behavior, around ~1041 erg s−1, above which the softer blackbody shows a sort of saturation, while the harder one still grows to a few times 1041 erg s−1, and a rather sharp correlation between temperature and radii of the blackbodies (R2 ∝ kT−3), which holds for the most luminous parts of the flares (~Ltot ≥ 1041 erg s−1). Within the magnetar model, the majority of these findings are accounted for in terms of thermalized emission from the E-mode and O-mode photospheres. Interestingly, the maximum observed luminosity coming from a region of ~15 km matches the magnetic Eddington luminosity at the same radius, for a surface dipole field of ~8 × 1014 G (virtually equal to that deduced from the spin-down of SGR 1900+14).

Supermassive Stars in Quasar Disks

We propose that supermassive stars may form in quasar accretion disks, and we discuss possible observational consequences. The structure and stability of very massive stars are reviewed. Because of high accretion rates, quasar disks are massive, and the fringes of their optically luminous parts are prone to fragmentation. Starting from a few hundred solar masses, a dominant fragment will grow to the isolation mass, which is a significant fraction of the disk mass, more quickly than the fragment contracts onto the stellar main sequence. A gap will form in the disk, and the star will migrate inward on the accretion timescale, which is comparable to the star's main-sequence lifetime. By interrupting the gas supply to the inner disk, the gap may temporarily dim and redden the quasar. The final stages of stellar migration will be a strong source of low-frequency gravitational waves.

The Size Evolution of High-Redshift Galaxies

Hubble Space Telescope images of high-redshift galaxies selected via color and photometric redshifts are used to examine the size and axial-ratio distribution of galaxies as a function of redshift at lookback times t > 8 Gyr. These parameters are measured at rest-frame UV wavelengths (1200-2000 Angstroms) on images with a rest-frame resolution of less than 0.8 kpc. Galaxy radii are found to scale with redshift approximately as the inverse of the Hubble parameter H(z). This is in accord with the theoretical expectation that the typical sizes of the luminous parts of galaxies should track the expected evolution in the virial radius of dark-matter halos. The mean ratio of semi-major to semi-minor axis for a bright well-resolved sample of galaxies at z ~ 4 is b/a = 0.65, suggesting that these Lyman break galaxies are not drawn from a spheroidal population. However the median concentration index of this sample is C = 3.5, which is closer to the typical concentration indices, C ~ 4, of nearby elliptical galaxies than to the values, C<2 for local disk galaxies of type Sb and later.

Damped Lyα Absorber and the Faint End of the Galaxy Luminosity Function at High Redshift

We combine predictions for several hierarchical cosmogonies with observational evidence on damped Lya systems (DLASs) to establish a correspondence between the high-redshift galaxy population and the properties of DLASs. We assume that high-redshift galaxies and damped Lya systems are hosted by the same dark matter halos and require consistency between the predicted halo space density, the rate of incidence and the velocity width distribution of damped Lya systems, and the observed galaxy lumi- nosity function at the bright end. We arrive at the following results: (1) predicted impact parameters between the damped absorption system and the luminous parts of the absorbing galaxy are expected to be very small for most galaxies; (2) luminosities of galaxies causing damped absorption are gen- (0A.3¨1A) erally fainter than and damped Lya systems are predicted to sample preferentially the outer m R 25, regions of galaxies at the faint end of the galaxy luminosity function at high redshift. Therefore, DLASs should currently provide the best probe of the progenitors of normal present-day galaxies. Subject headings: galaxies: kinematics and dynamicsgalaxies: structureintergalactic medium ¨ quasars: absorption lines

Galaxy formation.

It is argued that within the standard Big Bang cosmological model the bulk of the mass of the luminous parts of the large galaxies likely had been assembled by redshift z approximately 10. Galaxy assembly this early would be difficult to fit in the widely discussed adiabatic cold dark matter model for structure formation, but it could agree with an isocurvature version in which the cold dark matter is the remnant of a massive scalar field frozen (or squeezed) from quantum fluctuations during inflation. The squeezed field fluctuations would be Gaussian with zero mean, and the distribution of the field mass therefore would be the square of a random Gaussian process. This offers a possibly interesting new direction for the numerical exploration of models for cosmic structure formation.

Infrared Emission from Barred Spiral Galaxies

AbstractAmongst relatively undisturbed spiral galaxies of type ≤ Sc barred morphology is unquestionably associated with powerful mid- and Far-IR emission. On the other hand, even amongst early type galaxies, those with LFIR/LB &lt; 1/3 exhibit no association of high relative FIR luminosity with barred morphology, but some association of IR colors resembling those of star formation regions (SFRs). Amongst systems with LFIR/LB &lt; 0.1 this ratio may be anti-correlated with barredness. It appears that enhanced IR emission from those galaxies whose star formation rate is currently elevated by the the bar translates them into the group with higher FIR-to-optical luminosity ratios. Depletion of extended nearnuclear gas and dust, once the bar has swept up the currently-available supplies, may reduce the fraction of the background stellar radiation field which can be converted to FIR radiation in the inner, most luminous parts of the galaxy. Thus, after the starburst has subsided, such galaxies may be less FIR-luminous than unbarred systems. Several uncertainties remain: it is still not clear whether barred morphology is a necessary condition for the generation of a starburst in an otherwise undisturbed galaxy, while evidence as to the effect of differing bar strengths is conflicting.

Rotation of halos in open and closed universes - Differentiated merging and natural selection of galaxy types

Computer simulations are used here to study the properties of galactic halos formed from Gaussian initial density perturbations in both open and closed dark matter universes. It is shown that if galaxies form through gravitational collapse from initial, Gaussian density perturbations, then their luminous parts do not have the original values of either specific angular momentum (ellipticals) or spin parameter lambda (spirals). The rotational properties of a halo depend only weakly on either the halo density or the density of its environment. Variations of the large-scale density of the environment have an expected, dramatic effect on the density of individual halos. Dissipationless merging forces the cores of the merging objects into the core of the merger product. In the process, cores become more bound and lose angular momentum. These findings are extrapolated to propose a model for galaxy formation in which both ellipticals and spirals come into being through mergers. 59 references.

Structure and tip-opening of laminar diffusion flames

Using an enclosed cylindrical burner, laminar diffusion flames of hydrogen/methane/nitrogen mixtures have been probed for their temperature and stable species concentration profiles, and the tip opening phenomenon has been investigated experimentally. The results show that, with increasing height, the concentration of hydrogen becomes less than that of methane, and the ratio of hydrogen to methane, which should be constant in the case of equal diffusivities of hydrogen and methane, is also decreased. These results substantiate the higher diffusivity of hydrogen relative to methane, and further indicate that the preferential diffusion of hydrogen occurs not only at the tip region of strong flame curvature but also around the flame base where the directions of flow and diffusion are almost orthogonal. As the mixture is diluted considerably, the flame becomes separated into two luminous parts, and the upper part finally blows off from the peripheral part (i.e., the tip is opened), which seems to be caused by the accumulated effect of the preferential diffusion of hydrogen from the base. Once the tip is opened, not a small amount of unburned fuels (hydrogen and methane) and carbon monoxide is found to escape through the opened space. Concerned with this, a possible tip-opening mechanism based on the Damköhler number concept has been proposed. Furthermore, from this fact of fuel leakage and pollutant emission, it may be concluded that the occurrence of tip opening is undesirable in diffusion flame burning of mixed fuels such as hydrogen and hydrocarbons.

Numerical models of star formation in X-ray cluster cooling flows

A grid of numerical models is used here to study how accretion flows are affected by star formation. The observables associated with these models are investigated, presenting their X-ray surface brightness profiles. An X-ray diagnostic is searched for that, in the absence of spatially resolved X-ray spectral data, can be an unambiguous indicator for ongoing star formation in cooling flows. The spatial distributions of newly formed stars are presented and compared to profiles of the accreting galaxy in each model. Whether the accretion population can form the luminous parts of the accreting galaxy or whether it forms a dark component is considered.

Riometer absorption and spectral index for precipitating electrons with exponential spectra

The altitude profiles computed by Berger et al. (1974) for energy deposition in the atmosphere by electrons and electron‐produced X rays are transformed to electron density profiles in order to calculate the absorption of cosmic radio noise at 20, 30 and 51.4 MHz. The electrons are precipitated isotropic over the downward hemisphere with exponential spectra having e‐folding energies of 10, 50 and 200 keV. It is shown that the absorption of a wide angle (± 34°) riometer antenna is about 1.4 times larger than zenithal absorption, that a relationship A(ƒ) = k(ƒ)N0.45 exists between precipitation electron flux N and riometer absorption, with k(ƒ) a frequency dependent constant, and that the spectral index n, defined by A(ƒ) ∝ ƒ−n, is ≃2.0 for all three the e‐folding energies if the precipitation is uniform over the field of view of the antenna, but attains values well below 2.0 for the higher e‐folding energies only if the effective electron collision frequency is enhanced by hyperthermal electrons. The spectral index for wide beam riometer absorptions decreases also to values much less than 2.0 if a narrow strip of the upper atmosphere across the field of view is strongly ionized. It appears then that the frequency dependence of the absorption may not be related uniquely by A(ƒ) ∝ ƒ−n. The absorption event recorded at Sanae, Antarctica, on June 27, 1982, at 0122 not only illustrates that the spectral index n is not an unique parameter when electron precipitation is not uniform in the field of view of a riometer antenna but suggests also highly wavelength selective scattering of cosmic radio noise from the more luminous parts of the radio sky by the Bragg condition as suggested by D'Angelo (1976).

Cold dark matter, the structure of galactic haloes and the origin of the Hubble sequence

A popular theory for galaxy formation holds that the Universe is dominated by exotic particles such as axions, photinos or gravitinos (collectively known as cold dark matter, CDM)1–3. This hypothesis can reconcile the aesthetically pleasing idea of a flat universe with the standard theory of primordial nucleosynthesis and with upper limits on anisotropies in the cosmic microwave background4–6. The resulting model is consistent with the observed dynamics of galaxy clustering only if galaxy formation is biased towards high-density regions7,8. We have shown that such a biased model successfully matches the distribution of galaxies on megaparsec (Mpc) scales9. If it is to be viable, it must also account for the structure of individual galaxies and their haloes. Here we describe a simulation of a flat CDM universe which can resolve structures of comparable scale to the luminous parts of galaxies. We find that such a universe produces objects with the abundance and characteristic properties inferred for galaxy haloes. Our results imply that merging plays an important part in galaxy formation and suggest a possible explanation for the Hubble sequence.

Outstanding problems and instrumental prospects for the coming decade (A Review)

After a review of the discovery of external galaxies and the early classification of these enormous aggregates of stars into visually recognizable types, a new classification scheme is suggested based on a measurable physical quantity, the luminosity of the spheroidal component. It is argued that the new one-parameter scheme may correlate well both with existing descriptive labels and with underlying physical reality.Two particular problems in extragalactic research are isolated as currently most fundamental. (i) A significant fraction of the energy emitted by active galaxies (approximately 1% of all galaxies) is emitted by very small central regions largely in parts of the spectrum (microwave, infrared, ultraviolet and x-ray wavelengths) that were previously inaccessible to observation. The physical processes by which regions with less, similar 10(-9) the volume of the luminous stellar parts of galaxies produce such enormous quantities of energy are currently the subject of much speculative debate. (ii) It appears that most of the mass of ordinary galaxies resides far from the central luminous region, with the volume containing most of this mass greater, similar 10(3) times the volume containing most of the light-emitting stars; the nature, amount, and extent of this mass are quite unknown.New instruments that will be operating in the next decade and that may be helpful in solving these two problems are briefly mentioned with particular emphasis on the advances expected in angular resolution at wavelengths for which picture-taking ability has historically been poor or nonexistent.

Societies and Academies

PARIS. Academy of Sciences, August 16.—M. Janssen in the chair. —Note on the work recently carried out at the Observatory of Meudon, by M. J. Janssen. Special reference is made to the many successful solar photographs already obtained, representing the history of the solar disk for the last ten years. The processes are now so perfected that on the same plate the details are taken both of the brighter and less luminous parts, such as the edge of the disk and the penumbræ of the spots. Photographs ten times enlarged were exhibited of the extremely interesting spots taken on June 22, 1885, and last June. The striæ of the penumbra and the faculæ surrounding the former consist of granulations, in form and size resembling those constituting the entire solar surface. The same phenomenon reappears on the large round spot photographed last July, so that it seems all but demonstrated that the whole solar disk has a uniform constitution, and that the so-called granulations are in fact the constituent elements of every part of the surface of the sun.—Fresh researches on the relations existing between the chemical and mechanical work of the muscular tissue (continued), by M. A. Chauveau, with the co-operation of M. Kaufmann. Here a determination is made of the coefficient of the quantity of mechanical work produced by the muscles performing useful work in the physiological conditions of the normal state. By translating into absolute measurements the indications furnished by the dynamograph already referred to, it is shown that the muscular work performed may be estimated at about 31 to 35 millionths of calorie.—Some further remarks on the radicular nature of the stolons in Nephrolepis, by M. A. Trécul. In reply to M. Lachmann's recent note, the author again shows that these stolons are not stems or stalks, but true roots. No matter what their length, they never produce leaves, have always the structure of roots, and as they alone represent the primary roots of Nephrolepis, the expression “radicular stolons,” applied to them by the author, is fully justified.—New fluorescences with well-defined spectral rays (continued), by M. Lecoq de Boisbaudran. The author here treats fully the combination of alumina and the earth Zβ2O3, which, without being pure, is very rich in Zβ and poor in Zα. Alumina with 1/50 of this earth heated with sulphuric acid and moderately calcined shows a somewhat yellowish-green fluorescence, much more vivid than that of alumina containing the same quantity of Zα2O3 impure. The fluorescences have also been examined of calcined alumina containing the oxides of Ce, La, Er, Tu, Dy, Yb, Gd, Yt, and U. During these researches several rays were noticed apparently belonging to none of the already determined elementary bodies. Some of these rays may perhaps correspond to the substances announced by Mr. Crookes; but each case will have to be determined for itself.—Determination of the longitude of the Observatory of Tacubaya, Mexico, by MM. Anguiano and Pritchett. Continuous observations spread over six months show a definite longitude of 6h. 36m. 46.56s. west of Greenwich, which will require a correction of close upon 5s. for the accepted longitude of the capital of Mexico.—Electric excitement of the liver, by MM. Gréhant and Mislawsky. The question is discussed, whether the excitement of the liver by electricity increases the quantity of urea contained in the blood. In opposition to the views of M. Stolnikow the experiments here described show that variations in quantity occur only in the arterial blood, and that the blood of the supra-hepatic veins presents no change in the weight of the urea after electric excitement of the liver.—Dissemination of the Bacillus of tuberculosis by flies, by MM. Spilmann and Haushalter. Observations recently made in consumptive-hospitals seem to show that the virus (Koch's Bacillus) may easily be disseminated by the house-fly.—Note on Hæmatocytes. by M. Fokker. The author recently showed that the protoplasm taken from a healthy animal and protected from microbes survives and may produce fermentations. Here he continues his researches, showing that this protoplasm is capable of generating a vegetable form different from that under which it existed in the animal organism. But the Hæmatocytes thus produced do not multiply themselves in a cultivating medium, and their development should perhaps be described as a case of heterogeny.