Fog Computing: An Extension to the Cloud or the Future

Fog computing is a decentralized computing platform, which is an extension to cloud, computing. [2]The main aim of fog computing or fogging is to erase the difficulties in earlier platforms and guide the computation nearer to its data sources and data centers. A Reduction is noticed in latency and costs of delivering the data. This can be highlighted as a major advantage of this distributed platform.[1]This novel platform provides reliability, fault tolerance and security. With off-loading data centers and reducing service latency, this technology is very well suited for IoT applications. [1]The security and privacy have always been a major challenge to cloud computing and related technologies which are handled by Fogging. [2]By bringing computation close to data sources there are many field of aspects that are improved with help of Fog Computing. The paper presents the comparison of fog computing with other computing technologies

A taxonomic review of the subtribe Pericalina (Coleoptera: Carabidae: Lebiini) in the Western hemisphere : with descriptions of new species and notes about classification and zoogeography

A taxonomic review of the lebiine sub tribe Pericalina in the Western Hemisphere, this paper includes a treatment of the genus-groups, a key to the genera, keys to subgenera, species groups, and species of each polybasic genus, descriptions of new species and new subgenera, new locality records for previously described species, re-rankings, and new synonymy. In total, 111 species and subspecies are treated, 26 of which are described as new

The 90-day report for SL4 experiment S019: UV stellar astronomy

The use of Experiment S019 to obtain moderate dispersion stellar spectra extending down to 1300A with sufficient spectral resolution to permit the study of ultraviolet (UV) line spectra and of spectral energy distributions of early-type stars is studied. Data obtained from this experiment should be of sufficient accuracy to permit detailed physical analysis of individual stars and nebulae, but an even more basic consideration is the expectation of obtaining spectra of a sufficient number of stars so that a statistically meaningful survey may be made of the UV spectra of a wide variety of star types. These should include all luminosity classes of spectral types O, B and A, as well as peculiar stars such as Wolf-Rayet stars and Ap or Am stars. An attempt was also made to obtain, in the no-prism mode, low dispersion UV spectra in a number of Milky Way star fields and in nearby galaxies

Visual observations over oceans

Important factors in locating, identifying, describing, and photographing ocean features from space are presented. On the basis of crew comments and other findings, the following recommendations can be made for Earth observations on Space Shuttle missions: (1) flyover exercises must include observations and photography of both temperate and tropical/subtropical waters; (2) sunglint must be included during some observations of ocean features; (3) imaging remote sensors should be used together with conventional photographic systems to document visual observations; (4) greater consideration must be given to scheduling earth observation targets likely to be obscured by clouds; and (5) an annotated photographic compilation of ocean features can be used as a training aid before the mission and as a reference book during space flight

Cloud absorption radiometer

The Cloud Absorption Radiometer (CAR) was developed to measure spectrally how light is scattered by clouds and to determine the single scattering albedo, important to meteorology and climate studies, with unprecedented accuracy. This measurement is based on ratios of downwelling to upwelling radiation within clouds, and so is not strongly dependent upon absolute radiometric calibration of the instrument. The CAR has a 5-inch aperture and 1 degree IFOV, and spatially scans in a plane orthogonal to the flight vector from the zenith to nadir at 1.7 revolutions per second. Incoming light is measured in 13 spectral bands, using silicon, germanium, and indium-antimonide detectors. Data from each channel is digitally recorded in flight with 10-bit (0.1 percent) resolution. The instrument incorporates several novel features. These features are briefly detailed

Condensation on the outer surface of window glazings - Causes, effect on heat loss and method for prevention

Fogging on the outside surfaces of window glazings increases if the thermal insulation of the glazing is improved, i.e., the k value is decreased as realized in the heat-insulating glasses currently on the market. The main reason for this is the radiation exchange with the open sky. The most endangered Windows for fogging are the sky lights and glazings in the skin of buildings, e. g. structural glazing facades, because they are exposed to the largest portion of the open sky. The conditions of fogging are investigated and discussed, as well as its influence on the heat loss of glazings is demonstrated. By radiation exchange with the open sky, the heat loss of window glazings can be increased by more than a factor 2 in comparison to the standardized k value. However, fogging reduces heat losses in dependence on the outside air humidity. Fogging and heat loss can be considerably reduced by a low-emissive coating on the outer surface of glazings. The demands on such a coating are discussed. Also a method of double coating consisting of a low-emissive subcoating and a hydrophobic and anti-sticking top-coating is presented, which has a self-cleaning effect. Lowemissive and, at the same time, self-cleaning coatings, deposited on the outer surface of glazings are a new function of flat glass and may be a challenge to the glass industry in the next years

Research in space science. some results at smithsonian observing stations special report

Residuals in field-reduced satellite observations, statistics on cloud cover, photographing chemiluminescent trails, and confirmation of satellite objectives by observational method