This study measured the X-ray fluorescence spectra of chromium compounds with different oxidation states (Cr0, Cr3+, Cr6+) using a high-resolution crystal spectrometer. Second-order contributions like plasmon satellites were resolved below the main Kβ1,3 emission line. The intensities and energies of these satellites varied between the compounds. Specifically, the Kβ' satellite had higher intensity and was at a lower energy for Cr3+ compared to Cr6+ or Cr0. Similar trends were observed for other satellites like Kβ5. The results provide information about how chemical bonding affects X-ray emission spectra.
UCSD NANO 266 Quantum Mechanical Modelling of Materials and Nanostructures is a graduate class that provides students with a highly practical introduction to the application of first principles quantum mechanical simulations to model, understand and predict the properties of materials and nano-structures. The syllabus includes: a brief introduction to quantum mechanics and the Hartree-Fock and density functional theory (DFT) formulations; practical simulation considerations such as convergence, selection of the appropriate functional and parameters; interpretation of the results from simulations, including the limits of accuracy of each method. Several lab sessions provide students with hands-on experience in the conduct of simulations. A key aspect of the course is in the use of programming to facilitate calculations and analysis.
UCSD NANO 266 Quantum Mechanical Modelling of Materials and Nanostructures is a graduate class that provides students with a highly practical introduction to the application of first principles quantum mechanical simulations to model, understand and predict the properties of materials and nano-structures. The syllabus includes: a brief introduction to quantum mechanics and the Hartree-Fock and density functional theory (DFT) formulations; practical simulation considerations such as convergence, selection of the appropriate functional and parameters; interpretation of the results from simulations, including the limits of accuracy of each method. Several lab sessions provide students with hands-on experience in the conduct of simulations. A key aspect of the course is in the use of programming to facilitate calculations and analysis.
UCSD NANO 266 Quantum Mechanical Modelling of Materials and Nanostructures is a graduate class that provides students with a highly practical introduction to the application of first principles quantum mechanical simulations to model, understand and predict the properties of materials and nano-structures. The syllabus includes: a brief introduction to quantum mechanics and the Hartree-Fock and density functional theory (DFT) formulations; practical simulation considerations such as convergence, selection of the appropriate functional and parameters; interpretation of the results from simulations, including the limits of accuracy of each method. Several lab sessions provide students with hands-on experience in the conduct of simulations. A key aspect of the course is in the use of programming to facilitate calculations and analysis.
This is the plenary talk given by Prof Shyue Ping Ong at the 57th Sanibel Symposium held on St Simon's Island in Georgia, USA.
Abstract: Powered by methodological breakthroughs and computing advances, electronic structure methods have today become an indispensable toolkit in the materials designer’s arsenal. In this talk, I will discuss two emerging trends that holds the promise to continue to push the envelope in computational design of materials. The first trend is the development of robust software and data frameworks for the automatic generation, storage and analysis of materials data sets. The second is the advent of reliable central materials data repositories, such as the Materials Project, which provides the research community with efficient access to large quantities of property information that can be mined for trends or new materials. I will show how we have leveraged on these new tools to accelerate discovery and design in energy and structural materials as well as our efforts in contributing back to the community through further tool or data development. I will also provide my perspective on future challenges in high-throughput computational materials design.
37 Latest results from GRAAL collaboration - Chinese Physics C (HEP & NP), De...Cristian Randieri PhD
Latest results from GRAAL collaboration - Chinese Physics C (HEP & NP), December 2009, Vol. 33, N. 12, pp. 1249-1253, ISSN: 1674-1137, doi: 10.1088/1674-1137/33/12/032
di V. Vegna, V. Bellini, J. P. Bouquet, L. Casano, A. D'Angelo, J. P. Didelez, R. Di Salvo, A. Fantini, D. Franco, G. Gervino, F. Ghio, G. Giardina, B. Girolami, A. Giusa, M. Guidal, E. Hourany, A. S. Ignatov, R. Kunnel, A. Lapik, A. Lleres, P. Levi Sandri, F. Mammoliti, G. Mandaglio, M. Manganaro, M. Moricciani, A.N. Mushkarenkov, V. G. Nedorezov, C. Randieri, D. Rebreyend, N. V. Rudnev, G. Russo, C. Schaerf, M. L. Sperduto, M. C. Sutera, A. Turinge (2009)
Abstract
The GRAAL experimental set-up consists of a polarized and tagged photon beam that covers an energy range from a minimum of 600 MeV up to a maximum of 1500 MeV, of a liquid Hydrogen or Deuterium target and of the 4π Lagrange detector optimized for photon detection. It allows the study of pseudo-scalar and vector meson photoproduction on the nucleon in the energy range corresponding to the second and the third resonance regions. In the following, the σ beam asymmetries in η and π0 photoproduction on quasi-free nucleon are shown. Also single and double polarization observables in K+Λ photoproduction on free proton are shown; they are important to confirm the role of new or poorly known resonances in the 1900 MeV mass region.
UCSD NANO 266 Quantum Mechanical Modelling of Materials and Nanostructures is a graduate class that provides students with a highly practical introduction to the application of first principles quantum mechanical simulations to model, understand and predict the properties of materials and nano-structures. The syllabus includes: a brief introduction to quantum mechanics and the Hartree-Fock and density functional theory (DFT) formulations; practical simulation considerations such as convergence, selection of the appropriate functional and parameters; interpretation of the results from simulations, including the limits of accuracy of each method. Several lab sessions provide students with hands-on experience in the conduct of simulations. A key aspect of the course is in the use of programming to facilitate calculations and analysis.
NANO281 is the University of California San Diego NanoEngineering Department's first course on the application of data science in materials science. It is taught by Professor Shyue Ping Ong of the Materials Virtual Lab (http://www.materialsvirtuallab.org).
UCSD NANO 266 Quantum Mechanical Modelling of Materials and Nanostructures is a graduate class that provides students with a highly practical introduction to the application of first principles quantum mechanical simulations to model, understand and predict the properties of materials and nano-structures. The syllabus includes: a brief introduction to quantum mechanics and the Hartree-Fock and density functional theory (DFT) formulations; practical simulation considerations such as convergence, selection of the appropriate functional and parameters; interpretation of the results from simulations, including the limits of accuracy of each method. Several lab sessions provide students with hands-on experience in the conduct of simulations. A key aspect of the course is in the use of programming to facilitate calculations and analysis.
UCSD NANO 266 Quantum Mechanical Modelling of Materials and Nanostructures is a graduate class that provides students with a highly practical introduction to the application of first principles quantum mechanical simulations to model, understand and predict the properties of materials and nano-structures. The syllabus includes: a brief introduction to quantum mechanics and the Hartree-Fock and density functional theory (DFT) formulations; practical simulation considerations such as convergence, selection of the appropriate functional and parameters; interpretation of the results from simulations, including the limits of accuracy of each method. Several lab sessions provide students with hands-on experience in the conduct of simulations. A key aspect of the course is in the use of programming to facilitate calculations and analysis.
Detection of solar_like_oscillations_in_relies_of_the_milk_way_asteroseismolo...Sérgio Sacani
Asteroseismic constraints on K giants make it possible to infer radii, masses and ages of tens
of thousands of field stars. Tests against independent estimates of these properties are however
scarce, especially in the metal-poor regime. Here, we report the detection of solar-like
oscillations in 8 stars belonging to the red-giant branch and red-horizontal branch of the globular
cluster M4. The detections were made in photometric observations from the K2 Mission
during its Campaign 2. Making use of independent constraints on the distance, we estimate
masses of the 8 stars by utilising different combinations of seismic and non-seismic inputs.
When introducing a correction to the Δν scaling relation as suggested by stellar models, for
RGB stars we find excellent agreement with the expected masses from isochrone fitting, and
with a distance modulus derived using independent methods. The offset with respect to independent
masses is lower, or comparable with, the uncertainties on the average RGB mass
(4 − 10%, depending on the combination of constraints used). Our results lend confidence to
asteroseismic masses in the metal poor regime. We note that a larger sample will be needed
to allow more stringent tests to be made of systematic uncertainties in all the observables
(both seismic and non-seismic), and to explore the properties of RHB stars, and of different
populations in the cluster.
UCSD NANO 266 Quantum Mechanical Modelling of Materials and Nanostructures is a graduate class that provides students with a highly practical introduction to the application of first principles quantum mechanical simulations to model, understand and predict the properties of materials and nano-structures. The syllabus includes: a brief introduction to quantum mechanics and the Hartree-Fock and density functional theory (DFT) formulations; practical simulation considerations such as convergence, selection of the appropriate functional and parameters; interpretation of the results from simulations, including the limits of accuracy of each method. Several lab sessions provide students with hands-on experience in the conduct of simulations. A key aspect of the course is in the use of programming to facilitate calculations and analysis.
This is the plenary talk given by Prof Shyue Ping Ong at the 57th Sanibel Symposium held on St Simon's Island in Georgia, USA.
Abstract: Powered by methodological breakthroughs and computing advances, electronic structure methods have today become an indispensable toolkit in the materials designer’s arsenal. In this talk, I will discuss two emerging trends that holds the promise to continue to push the envelope in computational design of materials. The first trend is the development of robust software and data frameworks for the automatic generation, storage and analysis of materials data sets. The second is the advent of reliable central materials data repositories, such as the Materials Project, which provides the research community with efficient access to large quantities of property information that can be mined for trends or new materials. I will show how we have leveraged on these new tools to accelerate discovery and design in energy and structural materials as well as our efforts in contributing back to the community through further tool or data development. I will also provide my perspective on future challenges in high-throughput computational materials design.
37 Latest results from GRAAL collaboration - Chinese Physics C (HEP & NP), De...Cristian Randieri PhD
Latest results from GRAAL collaboration - Chinese Physics C (HEP & NP), December 2009, Vol. 33, N. 12, pp. 1249-1253, ISSN: 1674-1137, doi: 10.1088/1674-1137/33/12/032
di V. Vegna, V. Bellini, J. P. Bouquet, L. Casano, A. D'Angelo, J. P. Didelez, R. Di Salvo, A. Fantini, D. Franco, G. Gervino, F. Ghio, G. Giardina, B. Girolami, A. Giusa, M. Guidal, E. Hourany, A. S. Ignatov, R. Kunnel, A. Lapik, A. Lleres, P. Levi Sandri, F. Mammoliti, G. Mandaglio, M. Manganaro, M. Moricciani, A.N. Mushkarenkov, V. G. Nedorezov, C. Randieri, D. Rebreyend, N. V. Rudnev, G. Russo, C. Schaerf, M. L. Sperduto, M. C. Sutera, A. Turinge (2009)
Abstract
The GRAAL experimental set-up consists of a polarized and tagged photon beam that covers an energy range from a minimum of 600 MeV up to a maximum of 1500 MeV, of a liquid Hydrogen or Deuterium target and of the 4π Lagrange detector optimized for photon detection. It allows the study of pseudo-scalar and vector meson photoproduction on the nucleon in the energy range corresponding to the second and the third resonance regions. In the following, the σ beam asymmetries in η and π0 photoproduction on quasi-free nucleon are shown. Also single and double polarization observables in K+Λ photoproduction on free proton are shown; they are important to confirm the role of new or poorly known resonances in the 1900 MeV mass region.
UCSD NANO 266 Quantum Mechanical Modelling of Materials and Nanostructures is a graduate class that provides students with a highly practical introduction to the application of first principles quantum mechanical simulations to model, understand and predict the properties of materials and nano-structures. The syllabus includes: a brief introduction to quantum mechanics and the Hartree-Fock and density functional theory (DFT) formulations; practical simulation considerations such as convergence, selection of the appropriate functional and parameters; interpretation of the results from simulations, including the limits of accuracy of each method. Several lab sessions provide students with hands-on experience in the conduct of simulations. A key aspect of the course is in the use of programming to facilitate calculations and analysis.
NANO281 is the University of California San Diego NanoEngineering Department's first course on the application of data science in materials science. It is taught by Professor Shyue Ping Ong of the Materials Virtual Lab (http://www.materialsvirtuallab.org).
UCSD NANO 266 Quantum Mechanical Modelling of Materials and Nanostructures is a graduate class that provides students with a highly practical introduction to the application of first principles quantum mechanical simulations to model, understand and predict the properties of materials and nano-structures. The syllabus includes: a brief introduction to quantum mechanics and the Hartree-Fock and density functional theory (DFT) formulations; practical simulation considerations such as convergence, selection of the appropriate functional and parameters; interpretation of the results from simulations, including the limits of accuracy of each method. Several lab sessions provide students with hands-on experience in the conduct of simulations. A key aspect of the course is in the use of programming to facilitate calculations and analysis.
UCSD NANO 266 Quantum Mechanical Modelling of Materials and Nanostructures is a graduate class that provides students with a highly practical introduction to the application of first principles quantum mechanical simulations to model, understand and predict the properties of materials and nano-structures. The syllabus includes: a brief introduction to quantum mechanics and the Hartree-Fock and density functional theory (DFT) formulations; practical simulation considerations such as convergence, selection of the appropriate functional and parameters; interpretation of the results from simulations, including the limits of accuracy of each method. Several lab sessions provide students with hands-on experience in the conduct of simulations. A key aspect of the course is in the use of programming to facilitate calculations and analysis.
Detection of solar_like_oscillations_in_relies_of_the_milk_way_asteroseismolo...Sérgio Sacani
Asteroseismic constraints on K giants make it possible to infer radii, masses and ages of tens
of thousands of field stars. Tests against independent estimates of these properties are however
scarce, especially in the metal-poor regime. Here, we report the detection of solar-like
oscillations in 8 stars belonging to the red-giant branch and red-horizontal branch of the globular
cluster M4. The detections were made in photometric observations from the K2 Mission
during its Campaign 2. Making use of independent constraints on the distance, we estimate
masses of the 8 stars by utilising different combinations of seismic and non-seismic inputs.
When introducing a correction to the Δν scaling relation as suggested by stellar models, for
RGB stars we find excellent agreement with the expected masses from isochrone fitting, and
with a distance modulus derived using independent methods. The offset with respect to independent
masses is lower, or comparable with, the uncertainties on the average RGB mass
(4 − 10%, depending on the combination of constraints used). Our results lend confidence to
asteroseismic masses in the metal poor regime. We note that a larger sample will be needed
to allow more stringent tests to be made of systematic uncertainties in all the observables
(both seismic and non-seismic), and to explore the properties of RHB stars, and of different
populations in the cluster.
Todo mundo sabe que os raios produzidos pela Estrela da Morte em Guerra nas Estrelas não pode existir na vida real, porém no universo existem fenômenos que as vezes conseguem superar até a mais surpreendente ficção.
A galáxia Pictor A, é um desses objetos que possuem fenômenos tão espetaculares quanto aqueles exibidos no cinema. Essa galáxia localiza-se a cerca de 500 milhões de anos-luz da Terra e possui um buraco negro supermassivo no seu centro. Uma grande quantidade de energia gravitacional é lançada, à medida que o material cai em direção ao horizonte de eventos, o ponto sem volta ao redor do buraco negro. Essa energia produz um enorme jato de partículas que viajam a uma velocidade próxima da velocidade da luz no espaço intergaláctico, chamado de jato relativístico.
Para obter imagens desse jato, os cientistas usaram o Observatório de Raios-X Chandra, da NASA várias vezes durante 15 anos. Os dados do Chandra, apresentados em azul nas imagens, foram combinados com os dados obtidos em ondas de rádio a partir do Australia Telescope Compact Array, e são aparesentados em vermelho nas imagens.
Discrete and broadband electron acceleration in Jupiter’s powerful auroraSérgio Sacani
The most intense auroral emissions from Earth’s polar regions,
called discrete for their sharply defined spatial configurations, are
generated by a process involving coherent acceleration of electrons
by slowly evolving, powerful electric fields directed along the
magnetic field lines that connect Earth’s space environment to its
polar regions1,2. In contrast, Earth’s less intense auroras are generally
caused by wave scattering of magnetically trapped populations of
hot electrons (in the case of diffuse aurora) or by the turbulent or
stochastic downward acceleration of electrons along magnetic field
lines by waves during transitory periods (in the case of broadband
or Alfvénic aurora)3,4. Jupiter’s relatively steady main aurora has a
power density that is so much larger than Earth’s that it has been
taken for granted that it must be generated primarily by the discrete
auroral process5–7. However, preliminary in situ measurements of
Jupiter’s auroral regions yielded no evidence of such a process8–10.
Here we report observations of distinct, high-energy, downward,
discrete electron acceleration in Jupiter’s auroral polar regions. We
also infer upward magnetic-field-aligned electric potentials of up to
400 kiloelectronvolts, an order of magnitude larger than the largest
potentials observed at Earth11. Despite the magnitude of these
upward electric potentials and the expectations from observations
at Earth, the downward energy flux from discrete acceleration is less
at Jupiter than that caused by broadband or stochastic processes,
with broadband and stochastic characteristics that are substantially
different from those at Earth.
A mildly relativistic wide-angle outflow in the neutron-star merger event GW1...Sérgio Sacani
GW170817 was the first gravitational wave detection of a binary
neutron-star merger1
. It was accompanied by radiation across the
electromagnetic spectrum and localized2
to the galaxy NGC 4993
at a distance of 40 megaparsecs. It has been proposed that the
observed γ-ray, X-ray and radio emission is due to an ultrarelativistic
jet launched during the merger, directed away from
our line of sight3–6. The presence of such a jet is predicted from
models that posit neutron-star mergers as the central engines
that drive short hard γ-ray bursts7,8
. Here we report that the radio
light curve of GW170817 has no direct signature of an off-axis
jet afterglow. Although we cannot rule out the existence of a jet
pointing elsewhere, the observed γ-rays could not have originated
from such a jet. Instead, the radio data require a mildly relativistic
wide-angle outflow moving towards us. This outflow could be the
high-velocity tail of the neutron-rich material dynamically ejected
during the merger or a cocoon of material that breaks out when a
jet transfers its energy to the dynamical ejecta. The cocoon model
explains the radio light curve of GW170817 as well as the γ-rays
and X-rays (possibly also ultraviolet and optical emission)9–15, and
is therefore the model most consistent with the observational data.
Cocoons may be a ubiquitous phenomenon produced in neutronstar
mergers, giving rise to a heretofore unidentified population of
radio, ultraviolet, X-ray and γ-ray transients in the local Universe
The atacama cosmology_telescope_measuring_radio_galaxy_bias_through_cross_cor...Sérgio Sacani
A radiação cósmica de micro-ondas aponta para a matéria escura invisível, marcando o ponto onde jatos de material viajam a velocidades próximas da velocidade da luz, de acordo com uma equipe internacional de astrônomos. O principal autor do estudo, Rupert Allison da Universidade de Oxford apresentou os resultados no dia 6 de Julho de 2015 no National Astronomy Meeting em Venue Cymru, em Llandudno em Wales.
Atualmente, ninguém sabe ao certo do que a matéria escura é feita, mas ela é responsável por cerca de 26% do conteúdo de energia do universo, com galáxias massivas se formando em densas regiões de matéria escura. Embora invisível, a matéria escura se mostra através do efeito gravitacional – uma grande bolha de matéria escura puxa a matéria normal (como elétrons, prótons e nêutrons) através de sua própria gravidade, eventualmente se empacotando conjuntamente para criar as estrelas e galáxias inteiras.
Muitas das maiores dessas são galáxias ativas com buracos negros supermassivos em seus centros. Alguma parte do gás caindo diretamente na direção do buraco negro é ejetada como jatos de partículas e radiação. As observações feitas com rádio telescópios mostram que esses jatos as vezes se espalham por milhões de anos-luz desde a galáxia – mais distante até mesmo do que a extensão da própria galáxia.
Os cientistas esperam que os jatos possam viver em regiões onde existe um excesso de concentração da matéria escura, maior do que o da média. Mas como a matéria escura é invisível, testar essa ideia não é algo tão direto.
A magnetar-powered X-ray transient as the aftermath of a binary neutron-star ...Sérgio Sacani
Mergers of neutron stars are known to be associated with short γ-ray
bursts1–4
. If the neutron-star equation of state is sufficiently stiff
(that is, the pressure increases sharply as the density increases), at
least some such mergers will leave behind a supramassive or even a
stable neutron star that spins rapidly with a strong magnetic field5–8
(that is, a magnetar). Such a magnetar signature may have been
observed in the form of the X-ray plateau that follows up to half
of observed short γ-ray bursts9,10. However, it has been expected
that some X-ray transients powered by binary neutron-star mergers
may not be associated with a short γ-ray burst11,12. A fast X-ray
transient (CDF-S XT1) was recently found to be associated with a
faint host galaxy, the redshift of which is unknown13. Its X-ray and
host-galaxy properties allow several possible explanations including
a short γ-ray burst seen off-axis, a low-luminosity γ-ray burst at
high redshift, or a tidal disruption event involving an intermediatemass black hole and a white dwarf13. Here we report a second X-ray
transient, CDF-S XT2, that is associated with a galaxy at redshift
z = 0.738 (ref. 14). The measured light curve is fully consistent with
the X-ray transient being powered by a millisecond magnetar. More
intriguingly, CDF-S XT2 lies in the outskirts of its star-forming host
galaxy with a moderate offset from the galaxy centre, as short γ-ray
bursts often do15,16. The estimated event-rate density of similar
X-ray transients, when corrected to the local value, is consistent
with the event-rate density of binary neutron-star mergers that is
robustly inferred from the detection of the gravitational-wave event
GW170817.
A magnetar-powered X-ray transient as the aftermath of a binary neutron-star ...
By31503504
1. Prabhpreet kaur, Dr. Shashi Pandey / International Journal of Engineering Research and
Applications (IJERA) ISSN: 2248-9622 www.ijera.com
Vol. 3, Issue 1, January -February 2013, pp.503-504
Low Energy Plasmon Satellites in X-ray emission spectra of
Transition elements
Prabhpreet kaur*, Dr. Shashi Pandey**
(Department of Physics, CMJ University)
ABSTRACT
We have measured X-ray fluorescence used to accelerate protons and current of 1-2 μA was
spectra of 3d transition elements with high- applied. Chromium compound targets, pellets were
resolution crystal spectrometer. In order to study prepared. Lower beam current of the order of (28-
possible effects of chemical bonding in the 75nA) was used, so that target is not damaged
fluorescence spectra, we have measured different during proton bombardment.
chromium compounds. The Intensities and High-Resolution crystal spectrometer
energies relative to the parent diagram line were consists of a target holder, a slit, a diffraction crystal
determined. and a position detector.
Emitted photons were reflected in the first order by
Keywords: Chromium compounds, High 7.2×2.6 cm2 Lithium Fluoride plane crystal.
resolution X-ray spectroscopy, Proton excitation, Reflected photons were detected by Fuji imaging
second order radiative contributions. plate (IP).
The diffracted X-rays formed a 2D pattern
INTRODUCTION: on IP detector. The horizontal axis corresponds to
The diagram lines in the X-ray emission energy axis of spectrum. The vertical axis increases
spectra correspond to electron transitions in singly the collection area. A slit of width 1.1mm was used
ionized atoms. These diagram lines resemble atomic to get an experimental resolution close to the natural
one-electron level structure and are usually width of the observed spectral line. The distance
accompanied by the second order radiative between IP detector and the target was 858.6nm
contributions known as Satellites. Satellites which provided excellent angular resolution. As a
observed on lower energy side are called Lower result Kα1 line was achieved and second order
Energy Satellite (LES). Intensity of these lines contribution of Kβ1,3 diagram line was easily
depends directly on the type of excitation. This can resolved.
be explained by assuming that a Plasmon is excited Cr sample was divided into three groups
during X-ray emission, emitting energy ħɷp below Cr0 (Cr), Cr3+(Cr2O3) and Cr6+(K2CrO4) according to
the parent line. Plasmon satellites were initially its oxidation number. The influence of chemical
observed in L X-ray emission spectra of Na, Mg and structure on KβL1 and KMM lines was investigated.
Al. Later on in the kα emission of beryllium, The results of spectra analysis are listed in Table 1
graphite. Plasmon satellite exists due to sudden and 2.
disturbance of electron distribution.
If Plasmon exists in Solids during X-ray emissions Table 1: Intensities of second order contributions in
then High energy Satellite (HES) are observed. the Kβ1,3 fluorescence spectra of Cr compounds.
Line Cr Cr2O3 K2CrO4
EXPERIMENT: Kβ' 39.10±0.91 31.00±2.5 30.90±2.6
X-ray emission spectra either with proton L* 0.96±0.45
or photon excitation (.i.e. PIXE or XRF) are Kβ5 4.2±1.30 1.76±0.82 3.1±1.6
generally used for measurements and are very KβL1 5.20±0.35 6.05±0.54 3.03±0.92
effective for detecting low concentrations. The KMM 1.62±0.15 1.45±0.52 1.36±0.68
chemical state appears in the fine structure of the X-
ray spectra .It is expected that Kα1,2 spectra are free * stands for additional lines observed in case of
from chemical effects as they are emitted through K2CrO4 between Kβ1,3 and Kβ5 lines which was
transition between inner shells. Chemical effects are observed in the case of K2CrO4.
more pronounced to be found in Kβ1,3 spectra as The relative intensity for Kβ' line is given as I(Kβ')/
they are directly connected to 3d valence shell. I(Kβ1,3) Intensities are measured and given in %age.
In this work we have focused on 3d
transition element, Chromium (Cr).We have
measured significant chemical effects on the
Intensities and energies of LES.
The experiment was performed using High-
Resolution crystal spectrometer. 2Mev energy was
503 | P a g e
2. Prabhpreet kaur, Dr. Shashi Pandey / International Journal of Engineering Research and
Applications (IJERA) ISSN: 2248-9622 www.ijera.com
Vol. 3, Issue 1, January -February 2013, pp.503-504
Table 2: Energies (in eV) of second order relative to Kβ1,3 line. The same effect has been found
contributions in the Kβ1,3 fluorescence spectra of Cr for energy of KβL1 satellite line relative to Kβ1,3 line.
compounds relative to the Kβ1,3 diagram line.
Line Cr Cr2O3 K2CrO4 REFERENCES:
Kβ' -9.64±0.18 -11.6±0.34 -10.23±0.75 [1] P.Richard, B.Crasemann [Ed], Atomic
L* 28.90±1.3 Inner shell processes, Atomic Inner
Kβ5 42.2±1.2 36.4±1.2 43.1±1.8 ShellProcesses,Academic,New York,1975,
KβL1 52.85±0.32 52.25±0.40 55.92±0.64 P.99.
[2] C.S.Fadley, D.A.Shirley, Phys.Rev. A2
According to the results for the Kβ' line we can write (1970)(10)
down the following relations. [3] B.K.Agarwal, X-ray Spectroscopy,
I (Cr0) > I (Cr3+) (1) Springer Series optical sciences, 1979
I (Cr3+) ≥ I (Cr6+) (2) [4] R.Ferrell, Theory of positron Annihilation
δE (Cr3+) > δE (Cr6+) (3) in solids, Rev mod. Phys.28, 1959, 308-
δE (Cr6+) ≥ δE (Cr0) (4) 337.
Where I represents Intensity and δE represents [5] Surendra Poonia and S.N.Soni, Indian
energy position, relatively to the Kβ1,3 line. Journal of Pure and applied Physics ,
Similarly we can write down relations for Kβ5 line. Vol.45, Feb 2007 PP-119-126.
I (Cr0) ≥ I (Cr6+) (5) [6] K.S.Srivastava, S.P.Singh and R.L.
I (Cr6+) ≥ I (Cr3+) (6) Srivastava, Phys.Rev .B13 (1976), 3213.
δE (Cr0) > δE (Cr6+) (7) [7] Rud M.E. & Edward & Volz, D J,Phys
δE (Cr6+) ≥ δE (Cr3+) (8) Rev.151,(1966),28.
Where I represents intensity relative to sum of Kβ1,3 [8] M.Scrocco,Satellites in X-ray photo
and Kβ' lines. electron spectroscopy 32(1985)1307-1310.
δE represents energy position relative to the Kβ1,3 [9] K.Tsutsumi, H.Nakamori, J.Phys. Soc. Jpn
line. 25 (1968 )1418.
[10] S.I.Salem, G.M.Hockney, P.L.Lee, phys.
CONCLUSION: Rev A13 (1976) 330.
Proton induced Kβ1,3 x-ray fluorescence [11] S.D. Gamblin, D.S.Urch, J.Electron,
spectra of Cr have been measured with high Spectroscopy Related Phenomenon. 113
resolution crystal spectrometer. (2001) 179.
Second order contributions (Kβ', Kβ5, KβL1, [12] J.Tihara,T.omori, K.Yoshihara, K. Ishii,
KMM) were clearly resolved. We determined their Nucl.Instr.and Meth.B75 (1993) 32.
energies and intensities. This effect was found most [13] D.C.Lengreth, Phys.Rev. Letter, 26, 1229,
clearly pronounced in energy position of Kβ' line 1971.
[14] G.A.Rooke,Plasmon Satellites of soft X-
ray spectra, Phy letter 3,1963,34-36.
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