Peak Photon Energy Research Articles

Calculating the radiation characteristics of accelerated electrons in laser-plasma interactions

In this paper, we studied the characteristics of radiation emitted by electrons accelerated in a laser–plasma interaction by using the Lienard–Wiechert field. In the interaction of a laser pulse with a underdense plasma, electrons are accelerated by two mechanisms: direct laser acceleration (DLA) and laser wakefield acceleration (LWFA). At the beginning of the process, the DLA electrons emit most of the radiation, and the DLA electrons emit a much higher peak photon energy than the LWFA electrons. As the laser–plasma interaction progresses, the LWFA electrons become the major radiation emitter; however, even at this stage, the contribution from DLA electrons is significant, especially to the peak photon energy.

An all-optical Compton source for single-exposure x-ray imaging

All-optical Compton sources are innovative, compact devices to produce high energy femtosecond x-rays. Here we present results on a single-pulse scheme that uses a plasma mirror to reflect the drive beam of a laser plasma accelerator and to make it collide with the highly-relativistic electrons in its wake. The accelerator is operated in the self-injection regime, producing quasi-monoenergetic electron beams of around 150 MeV peak energy. Scattering with the intense femtosecond laser pulse leads to the emission of a collimated high energy photon beam. Using continuum-attenuation filters we measure significant signal content beyond 100 keV and with simulations we estimate a peak photon energy of around 500 keV. The source divergence is about 13 mrad and the pointing stability is 7 mrad. We demonstrate that the photon yield from the source is sufficiently high to illuminate a centimeter-size sample placed 90 centimeters behind the source, thus obtaining radiographs in a single shot.

A broadband gamma-ray spectrometry using novel unfolding algorithms for characterization of laser wakefield-generated betatron radiation.

We present a high-flux, broadband gamma-ray spectrometry capable of characterizing the betatron radiation spectrum over the photon energy range from 10 keV to 20 MeV with respect to the peak photon energy, spectral bandwidth, and unique discrimination from background radiations, using a differential filtering spectrometer and the unfolding procedure based on the Monte Carlo code GEANT4. These properties are experimentally verified by measuring betatron radiation from a cm-scale laser wakefield accelerator (LWFA) driven by a 1-PW laser, using a differential filtering spectrometer consisting of a 15-filter and image plate stack. The gamma-ray spectra were derived by unfolding the photostimulated luminescence (PSL) values recorded on the image plates, using the spectrometer response matrix modeled with the Monte Carlo code GEANT4. The accuracy of unfolded betatron radiation spectra was assessed by unfolding the test PSL data simulated with GEANT4, showing an ambiguity of less than 20% and clear discrimination from the background radiation with less than 10%. The spectral analysis of betatron radiation from laser wakefield-accelerated electron beams with energies up to 3 GeV revealed radiation spectra characterized by synchrotron radiation with the critical photon energy up to 7 MeV. The gamma-ray spectrometer and unfolding method presented here facilitate an in-depth understanding of betatron radiation from LWFA process and a novel radiation source of high-quality photon beams in the MeV regime.

GRB 140606B/iPTF14bfu: detection of shock-breakout emission from a cosmological γ-ray burst?

We present optical and near-infrared photometry of GRB~140606B ($z=0.384$), and optical photometry and spectroscopy of its associated supernova (SN). The results of our modelling indicate that the bolometric properties of the SN ($M_{\rm Ni} = 0.4\pm0.2$~M$_{\odot}$, $M_{\rm ej} = 5\pm2$~M$_{\odot}$, and $E_{\rm K} = 2\pm1 \times 10^{52}$ erg) are fully consistent with the statistical averages determined for other GRB-SNe. However, in terms of its $\gamma$-ray emission, GRB~140606B is an outlier of the Amati relation, and occupies the same region as low-luminosity ($ll$) and short GRBs. The $\gamma$-ray emission in $ll$GRBs is thought to arise in some or all events from a shock-breakout (SBO), rather than from a jet. The measured peak photon energy ($E_{\rm p}\approx800$ keV) is close to that expected for $\gamma$-rays created by a SBO ($\gtrsim1$ MeV). Moreover, based on its position in the $M_{V,\rm p}$--$L_{\rm iso,\gamma}$~plane and the $E_{\rm K}$--$\Gamma\beta$~plane, GRB~140606B has properties similar to both SBO-GRBs and jetted-GRBs. Additionally, we searched for correlations between the isotropic $\gamma$-ray emission and the bolometric properties of a sample of GRB-SNe, finding that no statistically significant correlation is present. The average kinetic energy of the sample is $\bar{E}_{\rm K} = 2.1\times10^{52}$ erg. All of the GRB-SNe in our sample, with the exception of SN 2006aj, are within this range, which has implications for the total energy budget available to power both the relativistic and non-relativistic components in a GRB-SN event.

A medium-energy photoemission and ab-initio investigation of cubic yttria-stabilised zirconia

Experimental and theoretical investigations into the electronic properties and structure of cubic yttria-stabilized zirconia are presented. Medium-energy x-ray photoemission spectroscopy measurements have been carried out for material with a concentration of 8-9 mol. % yttria. Resonant photoemission spectra are obtained for a range of photon energies that traverse the L2 absorption edge for both zirconium and yttrium. Through correlation with results from density-functional theory (DFT) calculations, based on structural models proposed in the literature, we assign photoemission peaks appearing in the spectra to core lines and Auger transitions. An analysis of the core level features enables the identification of shifts in the core level energies due to different local chemical environments of the constituent atoms. In general, each core line feature can be decomposed into three contributions, with associated energy shifts. Their identification with results of DFT calculations carried out for proposed atomic structures, lends support to these structural models. The experimental results indicate a multi-atom resonant photoemission effect between nearest-neighbour oxygen and yttrium atoms. Near-edge x-ray absorption fine structure spectra for zirconium and yttrium are also presented, which correlate well with calculated Zr- and Y-4d electron partial density-of-states and with Auger electron peak area versus photon energy curve.

INVESTIGATING THE <em>E</em><sub>p, i</sub> –<em>E</em><sub>iso</sub> CORRELATION

The correlation between the spectral peak photon energy, Ep, and the radiated energy or luminosity (i.e., the “Amati relation” and other correlations derived from it) is one of the central and most debated topics in GRB astrophysics, with implications for physics and the geometry of prompt emission, the identification and understanding of various classes of GRBs (short/long, XRFs,sub-energetic), and GRB cosmology. Fermi is exceptionally suited to provide, also in conjunction with Swift observations, a significant step forward in this field of research. Indeed, one of the main goals of Fermi/GBM is to make accurate measurements of Ep, by exploiting its unprecedented broad energy band from ~8 keV to ~30MeV; in addition, for a small fraction of GRBs, the LAT can extend the spectral measurements up to the GeV energy range, thus allowing a reliable estimate of the bolometric radiated energy/luminosity. We provide a review, an update and a discussion of the impact of Fermi observations in the investigation, understanding and testing of the Ep,i –Eiso (“Amati”) relation.

INVESTIGATING THE <em>E</em><sub>p, i</sub> –<em>E</em><sub>iso</sub> CORRELATION

The correlation between the spectral peak photon energy, <em>E</em>p, and the radiated energy or luminosity (i.e., the “Amati relation” and other correlations derived from it) is one of the central and most debated topics in GRB astrophysics, with implications for physics and the geometry of prompt emission, the identification and understanding of various classes of GRBs (short/long, XRFs,sub-energetic), and GRB cosmology. Fermi is exceptionally suited to provide, also in conjunction with Swift observations, a significant step forward in this field of research. Indeed, one of the main goals of Fermi/GBM is to make accurate measurements of <em>E</em>p, by exploiting its unprecedented broad energy band from ~8 keV to ~30MeV; in addition, for a small fraction of GRBs, the LAT can extend the spectral measurements up to the GeV energy range, thus allowing a reliable estimate of the bolometric radiated energy/luminosity. We provide a review, an update and a discussion of the impact of Fermi observations in the investigation, understanding and testing of the <em>E</em><sub>p,i</sub> –<em>E</em><sub>iso</sub> (“Amati”) relation.

On Amati Relation For GRB Prompt Emission

We propose a model for the spectral formation of Gamma Ray Burst (GRB) prompt emission, where the phenomenological Band function is usually applied to describe the GRB prompt emission. We suggest that the GRB prompt emission is mainly a result of the Comptonization of relatively soft photons of the star off electrons of a hot shell of plasma of temperature of the order of 109 K (or ~100 keV) that moves sub-relativistically with the bulk velocity substantially less than the speed of light. In this case, the Comptonization parameter is high and the interaction between a blackbody-like soft seed photon population and hot electrons leads to formation of a saturated Comptonization spectrum. We give an interpretation of the Amati relation between the intrinsic spectral peak photon energy and radiated energy or luminosity.

AN UPSCATTERING SPECTRAL FORMATION MODEL FOR THE PROMPT EMISSION OF GAMMA-RAY BURSTS

We propose a model for the spectral formation of Gamma Ray Burst (GRB) prompt emission, where the phenomenological Band's function is usually applied to describe the GRB prompt emission. We suggest that the GRB prompt emission is mainly a result of two upscattering processes. The first process is the Comptonization of relatively cold soft photons of the star off electrons of a hot shell of plasma of temperature T_e of the order of 10^{9} K (or kT_e~100 keV) that moves sub-relativistically with the bulk velocity V_b substantially less than the speed of light c. In this phase, the Comptonization parameter Y is high and the interaction between a blackbody-like soft seed photon population and hot electrons leads to formation of a saturated Comptonization spectrum modified by the sub-relativistic bulk outflow. The second process is an upscattering of the previously Comptonized spectrum by the plasma outflow once it becomes relativistic. This process gives rise to the high-energy power-law component above the peak in the EF(E)-diagram where F(E) is the energy flux. The latter process can be described by a convolution of the Comptonized spectrum with a broken-power-law Green function. Possible physical scenarios for this second upscattering process are discussed. In the framework of our model, we give an interpretation of the Amati relation between the intrinsic spectral peak photon energy and radiated energy or luminosity, and we propose a possible explanation of the GRB temporal variability.

FLARES IN THE CRAB NEBULA DRIVEN BY UNTWISTING MAGNETIC FIELDS

The recent discovery of PeV electrons from the Crab nebula, produced on rapid time scales of one day or less with a sharply peaked gamma-ray spectrum without hard X-rays, challenges traditional models of diffusive shock acceleration followed by synchrotron radiation. Here we outline an accleration model involving a DC electric field parallel to the magnetic field in a twisted toroidal field around the pulsar. Sudden developments of resistivity in localized regions of the twisted field are thought to drive the particle acceleration, up to PeV energies, resulting in flares. This model can reproduce the observed time scales of $T \approx 1$ day, the peak photon energies of $U_{\Phi,rr} \approx 1$ MeV, maximum electron energies of $U_{e,rr} \approx 1$ PeV, and luminosities of $L \approx 10^{36}$ erg s$^{-1}$.

Experimental Study of Silicon Monolayers for Future Extremely Thin Silicon-on-Insulator Devices: Phonon/Band Structures Modulation Due to Quantum Confinement Effects

We have experimentally studied Si monolayers, fabricated by thermal oxidation of silicon-on-insulator (SOI) substrates at high temperature, for future extremely thin SOI (ETSOI) complementary metal oxide semiconductor (CMOS) devices, and have shown the strong quantum confinement effects in the ETSOIs. We have successfully formed 0.52-nm Si monolayers, as confirmed by transmission electron microscopy (TEM) and a UV/visual reflection method. We have experimentally shown the asymmetric broadening and the peak downshift of the Raman peak of ETSOIs evaluated by UV-Raman spectroscopy, which is enhanced in the ETSOI thickness TSOI of less than about 5 nm. These results are due to the quantum phonon confinement effects in ETSOIs. Using the TEM observation and UV-Raman spectroscopy of ETSOIs, we have also shown the tensile strain of ETSOIs due to the Si bending and the TSOI variations in ETSOI substrates. In addition, we have observed photoluminescence (PL) from the ETSOIs with a TSOI of less than about 5 nm and the PL intensity strongly depends on the TSOI. However, the peak photon energy of about 1.85 eV in the PL spectrum is independent of the TSOI. We cannot explain the PL results perfectly at present, but we have introduced a possible three-region model of electron/hole pair generation in a two-dimensional Si layer and electron/hole pair recombination at the Si/SiO2 interface state region.

Experimental Study of Silicon Monolayers for Future Extremely Thin Silicon-on-Insulator Devices: Phonon/Band Structures Modulation Due to Quantum Confinement Effects

We have experimentally studied Si monolayers, fabricated by thermal oxidation of silicon-on-insulator (SOI) substrates at high temperature, for future extremely thin SOI (ETSOI) complementary metal oxide semiconductor (CMOS) devices, and have shown the strong quantum confinement effects in the ETSOIs. We have successfully formed 0.52-nm Si monolayers, as confirmed by transmission electron microscopy (TEM) and a UV/visual reflection method. We have experimentally shown the asymmetric broadening and the peak downshift of the Raman peak of ETSOIs evaluated by UV-Raman spectroscopy, which is enhanced in the ETSOI thickness TSOI of less than about 5 nm. These results are due to the quantum phonon confinement effects in ETSOIs. Using the TEM observation and UV-Raman spectroscopy of ETSOIs, we have also shown the tensile strain of ETSOIs due to the Si bending and the TSOI variations in ETSOI substrates. In addition, we have observed photoluminescence (PL) from the ETSOIs with a TSOI of less than about 5 nm and the PL intensity strongly depends on the TSOI. However, the peak photon energy of about 1.85 eV in the PL spectrum is independent of the TSOI. We cannot explain the PL results perfectly at present, but we have introduced a possible three-region model of electron/hole pair generation in a two-dimensional Si layer and electron/hole pair recombination at the Si/SiO2 interface state region.

COSMOLOGY WITH THE Ep,i – Eiso CORRELATION OF GAMMA–RAY BURSTS

Gamma–Ray Bursts (GRBs) are the brightest sources in the universe, emit mostly in the hard X–ray energy band and have been detected at redshifts up to about 8.2. Thus, they are in principle very powerful probes for cosmology. I shortly review the researches aimed to use GRBs for the measurement of cosmological parameters, which are mainly based on the correlation between spectral peak photon energy and total radiated energy or luminosity. In particular, based on an enriched sample of 120 GRBs, I will provide an update of the analysis by Amati et al. (2008) aimed at extracting information on ΩM and, to a less extent, on ΩΛ, from the E p,i – E iso correlation.

Epitaxial lateral overgrowth of InN by rf-plasma-assisted molecular-beam epitaxy

The orientation-dependent lateral growth of InN was studied and the epitaxial lateral overgrowth (ELO) of InN by rf-plasma-assisted molecular-beam epitaxy was demonstrated for the first time using stripe molybdenum (Mo)-mask-patterned sapphire (0001) substrates. Transmission electron microscopy observation revealed a high dislocation density of ∼5x10-9 cm-2 in the window region. By contrast, very few threading dislocations were observed in the wing region. In particular, there were no threading dislocations in the superficial layer of up to 3 μm width. An InN ELO sample exhibited narrow near-IR emission with a peak photon energy of 0.677 eV and a linewidth of 16.7 meV at 4 K.

Largely extended light-emission shift of ZnSe nanostructures with temperature

ZnSe nanowires and nanobelts with zinc blende structure have been synthesized. The morphology and the growth mechanisms of the ZnSe nanostructures will be discussed. From the photoluminescence (PL) of the ZnSe nanostructures, it is interesting to note that red color emission with only a single peak at the photon energy of 2 eV at room temperature is obtained while the typical bandgap transition energy of ZnSe is 2.7 eV. When the temperature is reduced to 150 K, the peak wavelength shifts to 2.3 eV with yellowish emission and then blue emission with the peak at 2.7 eV at temperature less than 50 K. The overall wavelength shift of 700 meV is obtained as compared to the conventional ZnSe of about 100 meV (i.e., sevenfold extension). The ZnSe nanostructures with enhanced wavelength shift can potentially function as visible light temperature-indicator. The color change from red to yellowish and then to blue is large enough for the nanostructures to be used for temperature-sensing applications. The details of PL spectra of ZnSe at various temperatures are studied from (i) the spectral profile, (ii) the half-width half-maximum, and (iii) the peak photon energy of each of the emission centers. The results show that the simplified configuration coordinate model can be used to describe the emission spectra, and the frequency of the local vibrational mode of the emission centers is determined.

Standardizing the gamma-ray bursts with the Amati Ep,i-Eiso relation: the updated Hubble diagram and implications for cosmography

The correlation between the peak photon energy of the internal spectrum Ep,i and isotropic equivalent radiated energy Eiso (the Amati relation) is explored in a scalar field model of dark energy. Using an updated data set of 109 high redshift GRBs, we show that the correlation parameters only weakly depend on the cosmological model. Once the parameters of Amati relation have been determined we use this relation to construct a fiducial GRBs Hubble diagram that extends up to redshifts ~ 8. Moreover we apply a local regression technique to estimate, in a model independent way, the distance modulus from the recently updated Union SNIa sample, containing 557 SNIa spanning the redshift range of 0.015 < z <1.55. The derived calibration parameters are used to construct an updated GRBs Hubble diagram, which we call the calibrated GRBs HD. We also compare the fiducial and calibrated GRBs HDs, which turned out to be fully statistically consistent, thus indicating that they are not affected by any systematic bias induced by the different calibration procedures. This means that the high redshift GRBs can be used to test different models of dark energy settling the circularity problem. Furthermore, we investigate possible evolutionary effects that might have important influence on our results. Our analysis indicates that the presently available GRBs datasets do not show statistically unambiguous evolutionary effect with the cosmological redshift. Finally we propose another approach to calibrate the GRB relations, by using an approximate luminosity distance relation, which holds in any cosmological model. We use this calibration of the Amati relation to construct an empirical approximate HD, which we compare with the calibrated GRBs HD. We finally investigate the implications of this approach for the high redshift cosmography.

Dislocation reduction via selective-area growth of InN accompanied by lateral growth by rf-plasma-assisted molecular-beam epitaxy

We investigated the selective-area growth (SAG) of InN by rf-plasma-assisted molecular-beam epitaxy using molybdenum (Mo)-mask-patterned sapphire (0001) substrates, which resulted in the formation of regularly arranged N-polar InN microcrystals. Transmission electron microscopy observation confirmed that the laterally grown side areas were nearly dislocation-free, although many threading dislocations (109–1010 cm−2) were generated at the InN/sapphire interface and propagated into the center of the InN microcrystals along the crystal c-axis. The laterally grown InN microcrystals exhibited narrow near-IR emission spectra with a peak photon energy of 0.627 eV and a linewidth of 39 meV at room temperature.

The correlation between peak photon energy and radiated energy in Gamma--Ray Bursts

The correlation between peak photon energy and radiated energy in Gamma--Ray Bursts

Temperature dependent photoluminescence of PECVD a-SiO x:H ( x

The temperature dependent visible photoluminescence (PL) property of a-SiO x :H ( x<2) samples prepared in a PECVD system by using SiH 4+CO 2 gas mixture is investigated at a temperature range of 20 K–400 K. One of the two explicitly distinguished PL bands, with varying peak photon energies between 1.70 and 2.05 eV, can be detected at only low temperatures below 200 K, which is attributed to tail-to-tail radiative recombination. Thermal quenching parameter ( T L ) of the tail-to-tail PL band is calculated as varying between 120 and 280 K as the atomic oxygen concentration ([O]at.%) of the samples increases. Stokes shift (Δ E Stokes ) of the tail-to-tail PL band is found to change from 85 meV to 420 meV due to band tail widening. The other PL band emerges at 2.1 eV and can be detected at higher temperatures with thermal activation behavior. The activation energies calculated about room temperature vary in the range of 8 meV–50 meV with oxygen concentration. Thermal activation of the 2.1 eV PL band is attributed to the behavior of thermally activated incoherent hopping migration of electrons. These electrons combine with self trapped holes (STHs) to form self trapped excitons (STEs). STEs are localized at intrinsic defects of SiO 2 structure such as oxygen vacancies ( E′ centers) and non-bridging oxygen hole centers (NBOHC).

Resist-less patterning on SiO2 by combination of X-ray exposure and vapor HF etching

We succeeded in a resist-less patterning of SiO2/Si substrates by a combination of X-ray exposure and vapor hydrogen fluoride (HF) etching. A 2 μm thick SiO2 layer was formed on a Si substrate by employing a thermal oxidation process. An X-ray mask consisted of a 1 μm thick Ta absorber on a 2 μm thick Si3N4 membrane mounted on a 1 mm thick Si frame, and a honeycomb pattern where 640 nm diameter circle dots arranged in the corners of a hexagon with a pitch of 960 nm was processed. X-ray exposure experiments were carried out on a beamline BL-4 with a peak photon energy of 2 keV at the TERAS synchrotron radiation (SR) facility. When a dose energy was 750 mAh, the transfer of the patterns was confirmed, although irradiations with different dose energy were also conducted. Moreover, heating temperatures and total etching times of SiO2/Si substrates in vapor HF etching were changed, and the shapes of etched patterns were observed by scanning electron microscope. It was learnt that an appropriate etching time existed between 30 and 60 min. Moreover, we observed discoloration of irradiated area by SR; and this seemed to be caused by changes in the etching rate of SiO2/Si substrates that led to the development of resist-less patterning technique.