scholarly journals X-ray irradiation of graphite solution from carbon rods of zinc-carbon battery wastes assisted by commercial detergent

2019 ◽  
Author(s):  
Wipsar Sunu Brams Dwandaru ◽  
Septiana Rahmawati ◽  
Rhyko Irawan Wisnuwijaya ◽  
Yusman Wiyatmo ◽  
Suparno ◽  
...  
Keyword(s):  
X Ray ◽  
Carbon Rods ◽  
Commercial Detergent

scholarly journals Synthesis of Carbon Nano Rods from Plastic Waste (PP) Using MgO AS A Catalyst

2020 ◽  
Vol 17 (2(SI)) ◽  
pp. 0609
Author(s):  
Amal Abbood et al.
Keyword(s):  
Pyrolysis Temperature ◽  
Surface Characteristics ◽  
Plastic Waste ◽  
Inert Gas ◽  
X Ray ◽  
Carbon Rods ◽  
Nano Rods ◽  
Short Time ◽  
Closed Reactor ◽  
Scanning Electron

    In this research, CNRs have been synthesized using pyrolysis of plastic waste(pp) at 1000 ° C for one hour in a closed reactor made from stainless steel, using magnesium oxide (MgO) as a catalyst. The resultant carbon nano rods were purified and characterized using energy dispersive X-ray spectroscopy (EDX), X-ray powder diffraction (XRD). The surface characteristics of carbon rods were observed with the Field emission scanning electron microscopy (FESEM). The carbon was evenly spread and had the highest concentration from SEM-EDX characterization. The results of XRD and FESEM have shown that carbon Nano rods (CNRs) were present in Nano figures, synthesized at 1000 ° C and with pyrolysis temperature 400° C. One of the advantages of this method is that using one reactor for a short time and without any use of inert gas as opposed to previous researches which used two reactors.

Synthesis Technique and Characterizations of Silver Nanostructures

2015 ◽  
Vol 14 (04) ◽  
pp. 1550012
Author(s):  
Shweta Rajawat ◽  
M. S. Qureshi
Keyword(s):  
Silver Nanoparticles ◽  
Electrolytic Deposition ◽  
Silver Nanostructures ◽  
Pure Silver ◽  
X Ray ◽  
Transmission Electron ◽  
Vis Spectroscopy ◽  
Two Samples ◽  
Carbon Rods

In this work, we report synthesis of nanostructures of silver nanoparticles using X-ray films. Exposed X-ray films, which consist of silver nanoparticles, are cut into small pieces of size 1 cm × 1 cm. These pieces were heated in distilled water at temperature 70°C. These nanoparticles, separated from heated films, are simultaneously collected through electrolytic deposition using copper and carbon rods. The carbon rod is wrapped over by Low density polyethylene (LDPE) sheet for easy extraction. This process was carried in two different environments (1) in broad daylight and (2) on a cloudy day. Characterization of the two samples was done using X-Ray Diffractometer (XRD), Transmission Electron Microscopy (TEM) and UV-Vis spectroscopy. XRD of the particles gave peaks well in accordance with JCPDS file 04-. This result confirms formation of highly pure silver nanoparticles. TEM revealed that the interaction of silver nanoparticles with sunlight gave chain like structures whereas in the absence of interaction with sunlight, cloudy day, nanoflowers were formed. Nanostructures were more prominent for bigger particles.

An efficient fulleride production system

1995 ◽  
Vol 73 (1-2) ◽  
pp. 38-44 ◽  
Author(s):  
W. R. Datars ◽  
S. Galts ◽  
T. Olech ◽  
P. K. Ummat
Keyword(s):  
Complete System ◽  
Continuous Production ◽  
Arc Furnace ◽  
X Ray Diffraction ◽  
High Quality ◽  
X Ray ◽  
Typical Data ◽  
Carbon Soot ◽  
Carbon Rods ◽  
Raman And Infrared Spectroscopy

A complete system for the production of the fullerides C60 and C70 is described. Emphasis is placed on efficient, continuous production of high-quality materials. Carbon soot with a content of 2–5% of a mixture of C60 and C70 is prepared from carbon rods with an arc furnace. The mixture is separated from the carbon by using a Soxhlet extractor. The C60 and C70 are separated with a chromotography column in which the solvent is cycled continuously. The separated C60 is purified by sublimation. The C70 is separated from heavier fullerides with a second chromotography procedure. Single crystals of C60 are prepared from pure C60 powder by slow sublimation. The C60 is characterized by mass spectroscopy, X-ray diffraction, and Raman and infrared spectroscopy. Typical data obtained with these techniques are shown.

Space and Time Distribution of Hard X-Ray Emission in a Loop at the Beginning of a Flare

1994 ◽  
Vol 144 ◽  
pp. 275-277
Author(s):  
M. Karlický ◽  
J. C. Hénoux
Keyword(s):  
Time Distribution ◽  
Electron Bombardment ◽  
Spatial Evolution ◽  
Superthermal Electrons ◽  
Flare Loop ◽  
X Ray ◽  
Superthermal Electron ◽  
Flare Loops ◽  
Chromospheric Evaporation ◽  
Temporal And Spatial

AbstractUsing a new ID hybrid model of the electron bombardment in flare loops, we study not only the evolution of densities, plasma velocities and temperatures in the loop, but also the temporal and spatial evolution of hard X-ray emission. In the present paper a continuous bombardment by electrons isotropically accelerated at the top of flare loop with a power-law injection distribution function is considered. The computations include the effects of the return-current that reduces significantly the depth of the chromospheric layer which is evaporated. The present modelling is made with superthermal electron parameters corresponding to the classical resistivity regime for an input energy flux of superthermal electrons of 109erg cm−2s−1. It was found that due to the electron bombardment the two chromospheric evaporation waves are generated at both feet of the loop and they propagate up to the top, where they collide and cause temporary density and hard X-ray enhancements.

Some Problems in Understanding the Solar Corona

1994 ◽  
Vol 144 ◽  
pp. 1-9
Author(s):  
A. H. Gabriel
Keyword(s):  
Solar Corona ◽  
Solar Atmosphere ◽  
Theoretical Modelling ◽  
Total System ◽  
Major Advance ◽  
X Ray ◽  
Proper Perspective ◽  
Space Observations

The development of the physics of the solar atmosphere during the last 50 years has been greatly influenced by the increasing capability of observations made from space. Access to images and spectra of the hotter plasma in the UV, XUV and X-ray regions provided a major advance over the few coronal forbidden lines seen in the visible and enabled the cooler chromospheric and photospheric plasma to be seen in its proper perspective, as part of a total system. In this way space observations have stimulated new and important advances, not only in space but also in ground-based observations and theoretical modelling, so that today we find a well-balanced harmony between the three techniques.

White-Light Coronal Structures: Streamers and CMEs

1994 ◽  
Vol 144 ◽  
pp. 82
Author(s):  
E. Hildner
Keyword(s):  
Emission Line ◽  
Electron Density ◽  
White Light ◽  
Coronal Mass Ejections ◽  
X Rays ◽  
Solar Cycles ◽  
Temperature Function ◽  
X Ray ◽  
Eclipse Observations ◽  
Coronal Structures

AbstractOver the last twenty years, orbiting coronagraphs have vastly increased the amount of observational material for the whitelight corona. Spanning almost two solar cycles, and augmented by ground-based K-coronameter, emission-line, and eclipse observations, these data allow us to assess,inter alia: the typical and atypical behavior of the corona; how the corona evolves on time scales from minutes to a decade; and (in some respects) the relation between photospheric, coronal, and interplanetary features. This talk will review recent results on these three topics. A remark or two will attempt to relate the whitelight corona between 1.5 and 6 R⊙to the corona seen at lower altitudes in soft X-rays (e.g., with Yohkoh). The whitelight emission depends only on integrated electron density independent of temperature, whereas the soft X-ray emission depends upon the integral of electron density squared times a temperature function. The properties of coronal mass ejections (CMEs) will be reviewed briefly and their relationships to other solar and interplanetary phenomena will be noted.

Iron K-Line Emission from X-Ray Binaries

1988 ◽  
Vol 102 ◽  
pp. 47-50
Author(s):  
K. Masai ◽  
S. Hayakawa ◽  
F. Nagase
Keyword(s):  
Accretion Disk ◽  
Radiative Recombination ◽  
Characteristic Temperature ◽  
Line Emission ◽  
Ionization Front ◽  
Continuum Radiation ◽  
X Ray ◽  
Low Mass ◽  
X Ray Binaries

AbstractEmission mechanisms of the iron Kα-lines in X-ray binaries are discussed in relation with the characteristic temperature Txof continuum radiation thereof. The 6.7 keV line is ascribed to radiative recombination followed by cascades in a corona of ∼ 100 eV formed above the accretion disk. This mechanism is attained for Tx≲ 10 keV as observed for low mass X-ray binaries. The 6.4 keV line observed for binary X-ray pulsars with Tx> 10 keV is likely due to fluorescence outside the He II ionization front.

Diagnostics of Gold Laser Plasmas

1988 ◽  
Vol 102 ◽  
pp. 357-360
Author(s):  
J.C. Gauthier ◽  
J.P. Geindre ◽  
P. Monier ◽  
C. Chenais-Popovics ◽  
N. Tragin ◽  
...  
Keyword(s):  
Experimental Results ◽  
Pure Gold ◽  
Electronic Temperature ◽  
X Ray ◽  
Laser Plasmas ◽  
Collisional Radiative Model ◽  
Radiative Model

AbstractIn order to achieve a nickel-like X ray laser scheme we need a tool to determine the parameters which characterise the high-Z plasma. The aim of this work is to study gold laser plasmas and to compare experimental results to a collisional-radiative model which describes nickel-like ions. The electronic temperature and density are measured by the emission of an aluminium tracer. They are compared to the predictions of the nickel-like model for pure gold. The results show that the density and temperature can be estimated in a pure gold plasma.

Axial Observation of X-Ray Spectra from a Beam-Foil Source

1988 ◽  
Vol 102 ◽  
pp. 339-342
Author(s):  
J.M. Laming ◽  
J.D. Silver ◽  
R. Barnsley ◽  
J. Dunn ◽  
K.D. Evans ◽  
...  
Keyword(s):  
Spectral Resolution ◽  
Heavy Ion ◽  
Ion Beams ◽  
Beam Axis ◽  
Doppler Broadening ◽  
X Ray ◽  
Beam Foil

AbstractNew observations of x-ray spectra from foil-excited heavy ion beams are reported. By observing the target in a direction along the beam axis, an improvement in spectral resolution, δλ/λ, by about a factor of two is achieved, due to the reduced Doppler broadening in this geometry.

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