Absorption Of Soft X-rays Research Articles

Investigation of Energy Deposition by Soft X-rays into Solar Cell Materials

A high-altitude nuclear detonation releases a significant portion of energy as X-rays with a blackbody spectrum. Satellites are particularly vulnerable to prompt soft X-rays (~1 keV) absorbed within a few microns of the surface of the solar array, causing melting and evaporation of its materials. The absorption of soft X-rays in solar cell materials is studied using GEANT4 computer software. Energy deposition as a function of depth (depth-dose profile) is calculated for slab geometries of dielectric and metallic materials. The photo-absorption and Compton scattering of X-rays and the contribution of secondary radiation, such as photo-electrons, Auger-electrons, and fluorescence photons are taken into account. The effect of the production of secondary radiation on the distribution of deposited dose in the near-surface region of materials is investigated. The results presented in this work are validated against published data and provide valuable insights into X-ray absorption by solar cell materials, the redistribution of energy by secondary radiation, and the spatial scale of power density deposition that can be used as a source term for the further thermomechanical analysis of a material’s phase transformations and melting.

Analysis of Bright Source Hardness Ratios in the 4 yr Insight-HXMT Galactic Plane Scanning Survey Catalog

We conduct a statistical analysis of the hardness ratio (HR) for bright sources in the 4 yr Galactic Plane Scanning Survey catalog of Insight-HXMT. Depending on the stable (variable) flux F s (F v) or spectrum S s(S v) of each source, the bright sources are classified into three groups: F v&S v, F v&S s, and F s&S s. Our study of the HR characteristics in different types of sources reveals that accretion-powered neutron star (NS) low-mass X-ray binaries (LMXBs) exhibit softer energy spectra than NS high-mass X-ray binaries (HMXBs), but harder energy spectra than black hole binaries in most cases. This difference is probably due to their different magnetic field strengths. Additionally, F v&S v LMXBs tend to be harder than F v&S s LMXBs below 7 keV, while the opposite is true for HMXBs. Our results suggest that LMXBs may dominate unclassified sources, and NS binaries are likely to be the primary type of X-ray binaries with ambiguous compact stars. By comparing the HR of transient sources in their outburst and low-flux states, it is found that the averaged HR of four sources in the two states are roughly comparable within uncertainties. We also investigate the spatial properties of the three groups and find that F v&S v sources are mainly located in the longitude of −20° < l < 9°, F v&S s sources cross the Galactic Plane, and F s&S s sources are predominantly concentrated in 19° < l < 42°. In addition, analyzing the HR spatial distributions shows the absorption of soft X-rays (primarily below 2 keV) in the Galactic Plane.

Study of the internal quantum efficiency of FBK sensors with optimized entrance windows

Single-photon detection of X-rays in the energy range of 250 eV to 1 keV is difficult for hybrid detectors because of the low quantum efficiency and low signal-to-noise ratio. The low quantum efficiency is caused by the absorption of soft X-rays in the entrance window of the silicon sensors. The entrance window consists of an insensitive layer on the surface and a highly doped layer, which is typically from a few hundred nanometers to a couple of micrometers thick and is comparable to the absorption depth of soft X-ray photons (e.g. the attenuation length of 250 eV X-ray photons is ∼100 nm in silicon). The low signal-to-noise ratio is mainly caused by the small signal amplitude (e.g. ca. 70 electrons for 250 eV X-ray photons in silicon) with respect to the electronic noise. To improve the quantum efficiency, the entrance window must be optimized by minimizing the absorption of soft X-rays in the insensitive layer, and reducing charge recombination at the Si-SiO2 interface and in the highly doped region. Low gain avalanche diodes (LGADs) with a multiplication factor between 5 and 10 increase the signal amplitude and therefore improve the signal-to-noise ratio for soft X-rays, enabling single-photon detection down to 250 eV. Combining LGAD technology with an optimized entrance window technology can thus allow hybrid detectors to become a useful tool also for soft X-ray detection. In this work we present the optimization of the entrance window by studying the internal quantum efficiency of eight different process technology variations. The sensors are characterized using light emitting diodes with a wavelength of 405 nm. At this wavelength, the light has an absorption depth of 125 nm, equivalent to that of 276 eV X-rays. The best variation achieves an internal quantum efficiency of 0.992 for 405 nm UV light. Based on this study, further optimization of the quantum efficiency for soft X-rays detection is planned.

Suzaku observation of the eclipsing high mass X-ray binary pulsar XTE J1855-026

We report results from analysis performed on an eclipsing supergiant high mass X-ray binary pulsar XTE J1855-026 observed with the X-ray Imaging Spectrometer (XIS) on-board Suzaku Observatory in April 2015. Suzaku observed this source for a total effective exposure of $$\sim $$ 87 ks just before an eclipse. Pulsations are clearly observed and the pulse profiles of XTE J1855-026 did not show significant energy dependence during this observation consistent with previous reports. The time averaged energy spectrum of XTE J1855-026 in the 1.0–10.5 keV energy range can be well fitted with a partial covering power law model modified with interstellar absorption along with a black-body component for soft excess and a gaussian for iron fluorescence line emision. The hardness ratio evolution during this observation indicated significant absorption of soft X-rays in some segments of the observation. For better understanding of the reason behind this, we performed time-resolved spectroscopy in the 2.5–10.5 keV energy band which revealed significant variations in the spectral parameters, especially the hydrogen column density and iron line equivalent width with flux. The correlated variations in the spectral parameters indicate towards the presence of clumps in the stellar wind of the companion star accounting for the absorption of low energy X-rays in some time segments.

Dynamics of space-charge acceleration of X-ray generated electrons emitted from a metal surface

The so-called vacuum space-charge acceleration of emitted electrons triggered by absorption of soft X-rays (a few 100eV) under intense near-infrared laser excitation is studied experimentally and theoretically. The influence of high excitation densities on the properties of Auger and photo electrons liberated by a probe X-ray beam is investigated for grazing-incidence photons interacting with an atomically clean Cu (111) surface as a model system. Transient electron spectra have been taken in a pump–probe setup at the BESSY II storage ring using a newly developed compact electrostatic retarding Bessel-box spectrometer. Strong electron-energy shifts have been found and assigned to space-charge acceleration. Model calculations based on experimental input parameters are in good agreement with experimentally obtained energy-gain values indicating ultimate limits of ultrafast X-ray experiments with photo or Auger electrons as a probe.

Influence of soft X-ray of a vacuum spark with laser initiation on the surface properties of solid solutions CdXHg1-XTe

At a certain form of broadband source soft X-ray spectrum is expected to achieve selective radiation exposure to one of the elements of a multi-component material CdXHg1-XTe. In this case we can talk about a change of the surface properties of the substance as a result of selective absorption of soft X-rays.

TheNuSTARview of the non-thermal emission from PSR J0437−4715

We present a hard X-ray NuSTAR observation of PSR J0437-4715, the nearest millisecond pulsar. The known pulsations at the apparent pulse period ~5.76 ms are detected at energies up to 20 keV. We measure a photon index $\Gamma= 1.65\pm0.24$ (90% confidence) for the power law fit to the non-thermal emission. It had been shown that spectral models with two or three thermal components fit the XMM-Newton spectrum of PSR J0437-4715, depending on the slope of the power-law component, and the amount of absorption of soft X-rays. The new constraint on the high-energy emission provided by NuSTAR removes ambiguities regarding the thermal components of the emission below 3 keV. We performed a simultaneous spectral analysis of the XMM-Newton and NuSTAR data to confirm that three thermal components and a power law are required to fit the 0.3-20 keV emission of PSR J0437-4715. Adding a ROSAT-PSPC spectrum further confirmed this result and allowed us to better constrain the temperatures of the three thermal components. A phase-resolved analysis of the NuSTAR data revealed no significant change in the photon index of the high-energy emission. This NuSTAR observation provides further impetus for future observations with the NICER mission (Neutron Star Interior Composition Explorer) whose sensitivity will provide much stricter constraints on the equation of state of nuclear matter by combining model fits to the pulsar's phase-folded lightcurve with the pulsar's well-defined mass and distance from radio timing observations.

Bright radio emission from an ultraluminous stellar-mass microquasar in M 31

A subset of ultraluminous X-ray sources (those with luminosities of less than 10(40) erg s(-1); ref. 1) are thought to be powered by the accretion of gas onto black holes with masses of ∼5-20M cicled dot, probably by means of an accretion disk. The X-ray and radio emission are coupled in such Galactic sources; the radio emission originates in a relativistic jet thought to be launched from the innermost regions near the black hole, with the most powerful emission occurring when the rate of infalling matter approaches a theoretical maximum (the Eddington limit). Only four such maximal sources are known in the Milky Way, and the absorption of soft X-rays in the interstellar medium hinders the determination of the causal sequence of events that leads to the ejection of the jet. Here we report radio and X-ray observations of a bright new X-ray source in the nearby galaxy M 31, whose peak luminosity exceeded 10(39) erg s(-1). The radio luminosity is extremely high and shows variability on a timescale of tens of minutes, arguing that the source is highly compact and powered by accretion close to the Eddington limit onto a black hole of stellar mass. Continued radio and X-ray monitoring of such sources should reveal the causal relationship between the accretion flow and the powerful jet emission.

Soft X-ray microscopy analysis of cell volume and hemoglobin content in erythrocytes infected with asexual and sexual stages of Plasmodium falciparum

Plasmodium falciparum, the most virulent agent of human malaria, undergoes both asexual cycling and sexual differentiation inside erythrocytes. As the intraerythrocytic parasite develops it increases in size and alters the permeability of the host cell plasma membrane. An intriguing question is: how is the integrity of the host erythrocyte maintained during the intraerythrocytic cycle? We have used water window cryo X-ray tomography to determine cell morphology and hemoglobin content at different stages of asexual and sexual differentiation. The cryo stabilization preserves native structure permitting accurate analyses of parasite and host cell volumes. Absorption of soft X-rays by protein adheres to Beer-Lambert's law permitting quantitation of the concentration of hemoglobin in the host cell compartment. During asexual development the volume of the parasite reaches about 50% of the uninfected erythrocyte volume but the infected erythrocyte volume remains relatively constant. The total hemoglobin content gradually decreases during the 48h cycle but its concentration remains constant until early trophozoite stage, decreases by 25%, then remains constant again until just prior to rupture. During early sexual development the gametocyte has a similar morphology to a trophozoite but then undergoes a dramatic shape change. Our cryo X-ray tomography analysis reveals that about 70% of the host cell hemoglobin is taken up and digested during gametocyte development and the parasite eventually occupies about 50% of the uninfected erythrocyte volume. The total volume of the infected erythrocyte remains constant, apart from some reversible shrinkage at stage IV, while the concentration of hemoglobin decreases to about 70% of that in an uninfected erythrocyte.

SUPERSOFT X-RAY PHASE OF SINGLE DEGENERATE TYPE Ia SUPERNOVA PROGENITORS IN EARLY-TYPE GALAXIES

In the single degenerate (SD) scenario for Type Ia supernova (SN Ia) progenitors, an accreting white dwarf (WD) is expected to undergo a supersoft X-ray source (SSS) phase. Recently, Gilfanov & Bogdan (2010, hereafter GB10) claimed that observed X-ray fluxes of early type galaxies would be too low to be consistent with the prediction of the SD scenario based on rather simple assumptions. We present realistic evolutionary models of SD systems and calculate durations of SSS phases. In most cases, accreting WDs spend a large fraction of time in the optically thick wind phase and the recurrent nova phase rather than the SSS phase. Thus the SSS phase lasts only for a few hundred thousand years. This is by a factor of ~10 shorter than those adopted by GB10 where the SN~Ia progenitor WD was assumed to spend most of its life as a SSS. The theoretical X-ray luminosity of the SSS has a large uncertainty because of the uncertain atmospheric model of mass-accreting WDs and absorption of soft X-rays by the companion star's cool wind material. We thus adopt an average of the observed fluxes of existing symbiotic SSSs, i.e., ~0.4 x 10^{36} erg s^{-1} for 0.3--0.7 keV. Using these SSS duration and soft X-ray luminosity, we show that the observed X-ray flux obtained by GB10 is rather consistent with our estimated flux in early type galaxies based on the SD scenario. This is a strong support for the SD scenario as a main-contributor of SNe Ia in early type galaxies.

γCassiopeiae: an X-ray Be star with personality

gamma Cassiopeiae (gCas) is a B0.5e star with peculiar X-ray emission properties and yet the prototype of its own small class. In this paper we examine the X-ray spectra for a 2004 XMM-Newton observation and a previously published 2001 Chandra observation. In both cases the spectra can be modeled with 3 or 4 thermal components, which appear be discrete in temperature and spatially distinct. The dominant component, having kT ~ 12 keV contributes most (~80-90%) of the flux. The secondary components have temperatures in the range of 2-3 keV to 0.1 keV; these values can shift in time. Importantly, we find that the strong absorption of soft X-rays in 2001 is absent in 2004, meaning that an absorbing column in front of the source has moved off the star or has been removed. Other differences include a reduced Fe abundance from the ionized lines of the FeKalpha complex (even more subsolar than the 2001 observation), a decrease of the Fe K and possibly of the Si K fluorescence features, and from the NVII and NeX H-alpha lines, a possible overabundance of N and Ne. Also, we note common characteristics in both spectra that seem to set gCas apart from HD110342, another member of this subclass studied in detail. In this sense these stars have different "personalities." For example, for gCas rapid X-ray flaring and slower changes in the light curve are only seldomly accompanied by variations in hardness, and the hot X-ray component remains nearly constant in temperature. Moreover, the light curve shows recurrent "lulls" in flux, suggesting that a relaxation cycle is operates as part of the (unknown) X-ray generation process.

Ablation process of silica glass induced by laser plasma soft X-ray irradiation

Silica glass can be machined by irradiation with laser plasma soft X-rays on nano- and micrometer scale. We have investigated the ablation process of silica glass induced by laser plasma soft X-ray irradiation. We observed ionic and neutral species emitted from silica surfaces after irradiation. Dominant ions and neutrals are O + and Si + ions and Si, O, SiO and Si 2 neutrals, respectively. The ions have kinetic energies of 13 and 25 eV, which are much higher than those of particles emitted by evaporation. The energy of laser plasma soft X-rays absorbed to silica glass at a fluence of 1.4 J/cm 2 is estimated to be 380 kJ/cm 3, which is higher than the binding energy of SiO 2 of 76 kJ/cm 3. These results suggest that the most of the bonds in silica glass are broken by absorption of laser plasma soft X-rays, that several percent of the atoms are ionized, and that neutral atoms are emitted together with repulsive ions. The process possibly enables us to fabricate nano structures.

Studies of ionic liquid solutions by soft X-ray absorption spectroscopy

Soft X-ray spectroscopies give specific information about the electronic structure around light elements. The high absorption of soft X-rays by almost every molecule, including air, requires studies under vacuum, which represents a great limitation. Solids with high vapor pressure and liquids are very difficult to be studied, making solution chemistry almost neglected. This work explores the use of ionic liquids, organic liquids with very low vapor pressure, as media to study chemical solutions using soft X-ray. N 1s spectra are reported of ionic liquid solutions of 1-methyl-3alkyl-imidazolium cation with different anions and chain lengths, and urea/choline chloride mixtures (a deep eutectic solvent) with several solutes including dyes (Janus Green B and Congo Red), synthetic polymers (polyaniline) and nitrate salts. While there are significant problems with the signal of the solvent, the results do show that it is possible to detect solute signals, and further to see spectral changes attributed to solvent–solute interactions.

Measurements of the xenon density in a pulsed jet from absorption of monochromatic soft X-rays

The density distribution in a pulsed xenon gas jet emanating through cylindrical and conic (supersonic) nozzles in vacuum was investigated experimentally and theoretically for different stagnation pressures and at different instants of time. The measurements were made from absorption of monochromatic soft X-rays (SXRs) (λ=13.6 nm) produced by a nanosecond laser-plasma source. Focusing normal-incidence multilayer mirrors were employed for the monochromatisation of soft X-rays and the production of transmission jet images (X-ray absorption patterns). Numerical simulations were made of the transient outflow of xenon in vacuum taking cluster production into account. The measured absolute density values and the density distribution agree nicely with the simulations.

X-ray Magnetic Circular Dichroism for Quantitative Element-Resolved Magnetic Microscopy

The use of X-ray magnetic circular dichroism in the absorption of soft X-rays for the layer-resolved imaging of magnetic domains is introduced. A photoelectron emission microscope, used as position-sensitive detector for electron yield detection of resonant absorption of circularly polarized X-rays at elemental absorption edges, enables the imaging of the magnetic microstructures at surfaces and buried magnetic layers. Extended to full-image local X-ray magnetic circular dichroism microspectroscopy, this combination of techniques allows the local microscopic determination of element-resolved spin and orbital magnetic moments.

Ionization statistics in silicon X-ray detectors — new experimental results

This paper presents a systematic experimental examination of the response of silicon detectors to the absorption of soft X-rays. Measurements in the single photon counting mode with detector structures — especially designed and produced for this purpose — exposed to monochromatized synchrotron radiation with energies between 300eV and 1400eV at room temperature as well as at 140 K are shown. A well-fitting semi-empirical model for the response function of detectors with implanted entrance windows is developed. It decomposes the measured spectra into a Gaussian peak representing the full X-ray energy and a low energy background caused by incomplete charge collection close to the detector surface. The energy and temperature dependence of the mean energy required for the generation of one electron hole pair is extracted from the experimental data. In addition to the already known dependence on the detector temperature it is shown that the pair creation energy is also a function of the photon energy.

Soft X-ray spectroscopy

X-ray spectrometry at low energies ( 12 A) presents special problems due to the inefficiency with which such X-rays are generated, the ease with which they are absorbed, and the difficulty of finding suitable dispersing elements. Advantage can, however, be taken of the ready absorption of these soft X-rays since their escape depth from most materials rarely exceeds one micron. Soft X-ray spectroscopy is therefore nanometer spectroscopy. Furthermore soft X-rays show large chemical effects which can be used to infer the chemical state of the emitting atom. The special problems associated with the production and dispersion of soft X-rays are considered in this paper together with methods for calculating the depth of X-ray production from surface layers

Mapping DNA and protein in biological samples using the scanning transmission x-ray microscope

The Scanning Transmission soft X-ray Microscope (STXM) at the XIA beamline at the National Synchrotron Light Source, Brookhaven National Laboratory, has achieved 50 nm Rayleigh resolution and has been used to image wet biological samples using the natural absorption differences between carbon and water in the water window (between carbon and oxygen K-absorption edges). The step-like jumps in the absorption of soft x-rays by materials as a function of energy have been used for elemental mapping. Examination of these absorption "edges" with high energy resolution resolves fine absorption structures. These fine structures are strongly affected by the atom's local environment, such that they carry detailed information about the atom's chemical state. We have used this chemical sensitivity to distinguish between materials which have similar elemental composition but are chemically different. Images with 50 nm resolution and spectra from a spot size less than (0.2 (μm)2 can be acquired routinely.Figure 1 shows the x-ray absorption fine structure spectra at the carbon absorption edge from DNA and bovine serum albumin (BSA, a typical protein) taken using the STXM.

An Experimental Method for Measuring the Heat Defect of Water Using Total Absorption of Soft X-Rays

The realization of the unit gray of the quantity absorbed dose to water by means of a water calorimeter requires knowledge of the heat defect to water, which is defined as the fraction of the radiation energy absorbed not appearing as heat. For low energy X-rays the heat defect can be determined by a method which uses total absorption of soft X-rays without involving absorbed dose measurements. The method described takes advantage of relative measurements allowing equal amounts of radiation energy to be absorbed in water or in a metal without heat defect. The method is outlined, the experimental set-up is described and the necessary corrections are discussed. Within the limits of uncertainty it is found that the pure water used in this study does not exhibit a heat defect.

Exponents in the Theory of the Soft X-Ray Threshold Anomaly of Heavy Alkali Metals

The threshold exponents α 0 of anomalous soft X-ray absorption spectra of heavy alkali metals in the theory of Nozières and De Dominicis are calculated. Special attention is paid on Cs where the value of α 0 is obtained experimentally as 0.06∼0.07 which is considerably smaller than α 0 for K and Rb. By a proposed model for Cs that the localized 4 f orbital is pulled in by the 5 p hole that is created by absorption of soft X-rays, resulting in the screening of the 5 p hole, we obtained the value of α 0 to be 0.05, in agreement qualitatively with the experimental results. For K and Rb, the obtained values for α 0 by the present study are 0.27 and 0.25, respectively, in satisfactory agreement with the experimental results.