Combustion Graphology Used To Improve Emulsions of Water-In-Heavy Fuel Oil,

Abstract Combustion graphology uses the infrared and luminous radiation of the flame and cenosphere of a burning droplet of heavy fuel oil in order to carry out scientific research with technical industrial applications. The rational combustion of the optimal water-heavy fuel oil emulsions in industrial power fumaces determines several advantages of which the most important is the de-pollution of the environment. Graphological testing for water-heavy fuel oil emulsion droplets is performed on a simulator and the result of the experiments is presented for two situations: when the effect of secondary atomisation is partially present and when the secondary atomisation is total, the whole droplet exploding. Experimental results are presented for samples processed in laboratory and in an industrial emulsifying installation. Generalities The combustion of mixtures of water (20%-30%) and heavy fuel oil, especially for attaining the reduction in smoke and soot emissions is a well-known method. Recently, this method was considerably improved in order to avoid the increase both of sulphur corrosive action and of the specific fuel consumption. First of all, it has been replaced the use of mixture of water and heavy fuel oil with emulsions, the water content in the emulsion being drastically reduced. Several beneficial advantages may be obtained by burning homogeneous emulsions of waterheavy fuel oil, with the water content limited to 3-6% [11, Due to the existence of a large number of various types of heavy fuel oil and emulsifying installations and in order to optimise the useful effects it is necessary to improve experimentally the quality of the water-heavy fuel oil emulsions. The emulsifying installations have adequate specific functioning rates; out of the range of these rates, the installation produces low quality emulsions, which are inappropriate to use. This work firstly gives explanations on what is the mechanism of the combustion of water-heavy fuel oil emulsions, the conclusions being based on experiments. The specific aspects of the droplet combustion graphology are herein set and a rapid and precise method for establishing the quality of waterheavy fuel oil emulsions is proposed. The validity of this method was verified in industrial and laboratory experiments. Some of these characteristic results are presented together with the applications of the combustion graphology method, which offers the possibility of fast and accurate processing of very economical activities in different fields. Secondary atomisation The meaning of the appearance of advantageous effects when using water-heavy fuel oil emulsions is related to the so-called secondary atomisation. If the water is finely dispersed into the fuel oil, the water droplets diameter is of the order of about 2-5 f.U' T1. During the primary atomisation process, these small water droplets will be incorporated into the oil droplets, the latter ones having a magnitude order of 20-150 11m. When the droplets enter the incandescent combustion chamber, they are heated up and a sudden vaporisation of the water droplets occurs, leading to a further atomisation of the oil droplets into smaller ones. The result is the secondary atomisation, produced by micro-explosions, which appear as a consequence of the important increase of the vapour pressure caused by the release of fine water droplets from the emulsion. As a conclusion, many constituents are released from the combustible mass of the fuel droplet. These components need a lower time to bum. The important decrease of the QIRT 96 -Eurotherm Series 50 -Edizioni ETS, Pisa 1997 http://d

An upper limit to the photon fraction in cosmic rays above 10^19 eV from the Pierre Auger Observatory

An upper limit of 16% (at 95% c.l.) is derived for the photon fraction in cosmic rays with energies above 10^19 eV, based on observations of the depth of shower maximum performed with the hybrid detector of the Pierre Auger Observatory. This is the first such limit on photons obtained by observing the fluorescence light profile of air showers. This upper limit confirms and improves on previous results from the Haverah Park and AGASA surface arrays. Additional data recorded with the Auger surface detectors for a subset of the event sample, support the conclusion that a photon origin of the observed events is not favoured

The effect of the geomagnetic field on cosmic ray energy estimates and large scale anisotropy searches on data from the Pierre Auger Observatory

We present a comprehensive study of the influence of the geomagnetic field on the energy estimation of extensive air showers with a zenith angle smaller than $60^\circ$, detected at the Pierre Auger Observatory. The geomagnetic field induces an azimuthal modulation of the estimated energy of cosmic rays up to the ~2% level at large zenith angles. We present a method to account for this modulation of the reconstructed energy. We analyse the effect of the modulation on large scale anisotropy searches in the arrival direction distributions of cosmic rays. At a given energy, the geomagnetic effect is shown to induce a pseudo-dipolar pattern at the percent level in the declination distribution that needs to be accounted for.Comment: 20 pages, 14 figure

Upper Limit on the Diffuse Flux of UHE tau neutrinos from the Pierre Auger Observatory.

The surface detector array of the Pierre Auger Observatory is sensitive to Earth-skimming tau-neutrinos $\nu_\tau$ that interact in the Earth's crust. Tau leptons from $\nu_\tau$ charged-current interactions can emerge and decay in the atmosphere to produce a nearly horizontal shower with a significant electromagnetic component. The data collected between 1 January 2004 and 31 August 2007 is used to place an upper limit on the diffuse flux of $\nu_\tau$ at EeV energies. Assuming an $E_\nu^{-2}$ differential energy spectrum the limit set at 90 % C.L. is $E_\nu^{2} \mathrm{d}N_{\nu_\tau}/\mathrm{d}E_{\nu} < 1.3 \times 10^{-7}$ GeV cm$^{-2}$ s$^{-1}$ sr$^{-1}$ in the energy range $2\times10^{17} \mathrm{eV} < E_\nu < 2\times10^{19}$ eV.Comment: 14 pages, 3 figure

The Pierre Auger Observatory scaler mode for the study of solar activity modulation of galactic cosmic rays

Since data-taking began in January 2004, the Pierre Auger Observatory has been recording the count rates of low energy secondary cosmic ray particles for the self-calibration of the ground detectors of its surface detector array. After correcting for atmospheric effects, modulations of galactic cosmic rays due to solar activity and transient events are observed. Temporal variations related with the activity of the heliosphere can be determined with high accuracy due to the high total count rates. In this study, the available data are presented together with an analysis focused on the observation of Forbush decreases, where a strong correlation with neutron monitor data is found.K.B. Barber... J.A. Bellido... R.W. Clay... M.J. Cooper... B.R. Dawson... A.E. Herve... V.C. Holmes... J. Sorokin... P. Wahrlich... B.J. Whelan... M.G. Winnick... et al., [for] The Pierre Auger collaboratio

The Pierre Auger Observatory scaler mode for the study of solar activity modulation of galactic cosmic rays

Since data-taking began in January 2004, the Pierre Auger Observatory has been recording the count rates of low energy secondary cosmic ray particles for the self-calibration of the ground detectors of its surface detector array. After correcting for atmospheric effects, modulations of galactic cosmic rays due to solar activity and transient events are observed. Temporal variations related with the activity of the heliosphere can be determined with high accuracy due to the high total count rates. In this study, the available data are presented together with an analysis focused on the observation of Forbush decreases, where a strong correlation with neutron monitor data is found.K.B. Barber... J.A. Bellido... R.W. Clay... M.J. Cooper... B.R. Dawson... A.E. Herve... V.C. Holmes... J. Sorokin... P. Wahrlich... B.J. Whelan... M.G. Winnick... et al., [for] The Pierre Auger collaboratio