The X-Ray Spectrum of Sco XR-1 to 100 keV

1968 ◽  
Vol 1 (4) ◽  
pp. 169-171
Author(s):  
P. J. N. Davison
Keyword(s):  
High Energy ◽  
The Other ◽  
Balloon Flight ◽  
X Ray

This paper presents the results of a measurement of the high-energy (E ≥ 17 keV) X-ray flux from Sco XR-1 extending to higher energies than has previously been reported. The measurement was made during a balloon flight launched from Mildura, Australia, on 29 February 1968. The X-ray observatory contained two independent X-ray detectors, one being similar in principle to the active collimator detector pioneered by Peterson et al., the other being basically similar to the graded shield detector developed by Boldt et al. Our two detecting systems are described in more detail by Buselli et al. and also in previous papers of this conference.

Growth of Transition Metal Films on AL(110) Surfaces

1995 ◽  
Vol 399 ◽  
Author(s):  
R.J. Smith ◽  
Adli A. Saleh ◽  
V. Shutthanandan ◽  
N.R. Shivaparan ◽  
V. Krasemann
Keyword(s):  
High Energy ◽  
Metal Films ◽  
Surface Strain ◽  
The Other ◽  
Photoemission Spectroscopy ◽  
Alloy Formation ◽  
Ion Scattering ◽  
X Ray ◽  
Photoelectron Diffraction ◽  
Ti Films

ABSTRACTThe growth of thin Pd, Ni, Fe and Ti films on Al(110) surfaces has been studied using high-energy ion scattering (HEIS), x-ray photoemission spectroscopy and photoelectron diffraction techniques. Of these four metals, only Ti grows as an epitaxial overlayer, while the other metals mix with the substrate to form surface alloys. In the HEIS experiments the backscattered ion yield from Al surface atoms is measured as a function of metal coverage on the Al surface. A decrease in the Al scattering is observed for Ti deposition while the other metals result in increased Al scattering, attributed to alloy formation. An explanation for the exceptional growth behavior of Ti on Al is provided using a model of surface strain associated with aluminide formation.

High-altitude balloon flight of CdZnTe detectors for high-energy x-ray astronomy

1998 ◽  
Author(s):  
Kimberly R. Slavis ◽  
Paul F. Dowkontt ◽  
Fred Duttweiller ◽  
John W. Epstein ◽  
Paul L. Hink ◽  
...  
Keyword(s):  
High Altitude ◽  
High Energy ◽  
Balloon Flight ◽  
X Ray ◽  
Cdznte Detectors

The Detection of High-Energy X-Rays from Ara XR-1 and Nor XR-1

1968 ◽  
Vol 1 (4) ◽  
pp. 165-166
Author(s):  
R. M. Thomas
Keyword(s):  
Zenith Angle ◽  
High Energy ◽  
Azimuth Angle ◽  
Field Of View ◽  
X Rays ◽  
Balloon Flight ◽  
X Ray ◽  
Energy Channels

This paper presents observations of weak X-ray sources at photon energies between 20 and 100 keV which were made during a balloon flight conducted from Mildura, Australia on 29 February 1968. Results obtained from Sco XR-1 and the Sagittarius region during this flight have been presented elsewhere, and here we report additional results obtained during a search of an area of sky in which several sources have been reported from rocket experiments at photon energies below about 10 keV. The detector used was an actively collimated and shielded NaI(T1) crystal, 2 mm thick and 54.3 cm2 in area. Incident photons were sorted into 16 energy channels between 7 and 167 keV (1.76 to 0.07 Å). The collimator field of view was 8°FWHM; the telescope axis was fixed at a zenith angle of 32° and its azimuth angle was varied by rotating the observatory below the balloon. This allowed the telescope to scan back and forth in azimuth across a source, the azimuth angle at any time being indicated by magnetometers.

scholarly journals High-Energy X-Ray Compton Scattering Imaging of 18650-Type Lithium-Ion Battery Cell

2019 ◽  
Vol 4 (3) ◽  
pp. 66 ◽  
Author(s):  
Kosuke Suzuki ◽  
Ari-Pekka Honkanen ◽  
Naruki Tsuji ◽  
Kirsi Jalkanen ◽  
Jari Koskinen ◽  
...  
Keyword(s):  
Energy Spectrum ◽  
Lithium Ion Battery ◽  
Compton Scattering ◽  
Present Method ◽  
Large Scale ◽  
Lithium Ion ◽  
High Energy ◽  
The Other ◽  
Battery Cell ◽  
X Ray

High-energy synchrotron X-ray Compton scattering imaging was applied to a commercial 18650-type cell, which is a cylindrical lithium-ion battery in wide current use. By measuring the Compton scattering X-ray energy spectrum non-destructively, the lithiation state in both fresh and aged cells was obtained from two different regions of the cell, one near the outer casing and the other near the center of the cell. Our technique has the advantage that it can reveal the lithiation state with a micron-scale spatial resolution even in large cells. The present method enables us to monitor the operation of large-scale cells and can thus accelerate the development of advanced lithium-ion batteries.

High-altitude balloon flight of CdZnTe detectors for high-energy x-ray astronomy: II

1999 ◽  
Author(s):  
Kimberly R. Slavis ◽  
Paul F. Dowkontt ◽  
Fred Duttweiller ◽  
John W. Epstein ◽  
Paul L. Hink ◽  
...  
Keyword(s):  
High Altitude ◽  
High Energy ◽  
Balloon Flight ◽  
X Ray ◽  
Cdznte Detectors

Effects of High Energy Ion Irradiation on Crystallization of Amorphous Germanium Films Deposited on Calcium Fluoride Substrates

1995 ◽  
Vol 396 ◽  
Author(s):  
Setsuo Nakao ◽  
Kazuo Saitoh ◽  
Masami Ikeyama ◽  
Hiroaki Niwa ◽  
Seita Tanemura ◽  
...  
Keyword(s):  
Thin Film ◽  
Calcium Fluoride ◽  
Structural Changes ◽  
Rutherford Backscattering Spectrometry ◽  
Ion Irradiation ◽  
High Energy ◽  
The Other ◽  
Ion Current ◽  
X Ray Diffraction ◽  
X Ray

AbstractAmorphous (a-) Ge films were deposited on air-cleaved CaF2 (111) substrates at different deposition temperatures (Td). The films were irradiated with 0.9 MeV Ge or Si ions at low ion current intensity (1c) l00nA/cm2. Their structural changes were studied by Rutherford backscattering spectrometry (RBS) -channeling technique and thin film x-ray diffraction (XRD) measurement. It was found that the films were epitaxially crystallized by Ge and Si ion irradiation although they included randomly oriented grains. Ge ion irradiation was more effective for the crystallization than Si ion irradiation. However, the amount of the randomly oriented grains was slightly higher when using Ge ions. On the other hand, ion irradiation to the films prepared at high Td also exhibited higher incidence of randomly oriented grains.

High Energy γ-ray Observations of SN 1987A

1988 ◽  
Vol 7 (4) ◽  
pp. 486-489
Author(s):  
R.K. Sood ◽  
J.A. Thomas ◽  
L. Waldron ◽  
R.K. Manchanda ◽  
G.K. Rochester ◽  
...  
Keyword(s):  
High Energy ◽  
Balloon Flight ◽  
X Ray ◽  
Preliminary Results ◽  
Sn 1987A ◽  
Γ Ray

AbstractSN 1987A has been observed with a combined high energy γ-ray (50-500 MeV) and hard X-ray (15-150 keV) payload during a balloon flight on 5 April 1988 from Alice Springs, Australia. The γ-ray observations, along with our earlier ones on 19 April 1987 are the only such observations of the supernova to date. The γ-ray detector characteristics are described. The preliminary results of the recent flight and their implications in terms of the known supernova parameters are discussed.

Observations of High-Energy X-Rays from Sagittarius

1968 ◽  
Vol 1 (4) ◽  
pp. 166-168
Author(s):  
M. C. Clancy
Keyword(s):  
Photon Energy ◽  
Scintillation Detector ◽  
Positional Information ◽  
High Energy ◽  
The Other ◽  
Opening Angle ◽  
X Rays ◽  
Balloon Flight ◽  
The Galaxy ◽  
Narrow Opening

During a recent balloon flight from Mildura, Australia, the region of the Galaxy between −10° < lII < +20°; −5° < bII< +5° was surveyed for high-energy X-rays of photon energy > 17 keV (λ < 0.7 Å) using an active collimation scintillation detector described elsewhere. The narrow opening angle of the telescope enables two sources to be resolved in this region of the sky. The position of one of these sources agrees well with the source GX3+1 observed at rocket wavelength by Bradt et al. while the other source is probably the same as that observed by Gursky et al. and designated GX−5.6. We present herein improved positional information for this latter source which hereafter will be designated GX354−5.

scholarly journals THE ASTRO-H MISSION

2013 ◽  
Vol 53 (A) ◽  
pp. 803-806
Author(s):  
Yoshitomo Maeda ◽  
Tadayuki Takahashi ◽  
Kazuhisa Mitsuda ◽  
Richard Kelley
Keyword(s):  
Spectral Resolution ◽  
High Sensitivity ◽  
High Energy ◽  
The Other ◽  
High Spectral Resolution ◽  
High Energy Astrophysics ◽  
Extended Source ◽  
X Ray ◽  
Imaging Capability ◽  
Wide Energy

A review of the Astro-H mission is presented here on behalf of the Astro-H collaboration. The joint JAXA/NASA ASTRO-H mission is the sixth in a series of highly successful X-ray missions initiated by the Institute of Space and Astronautical Science (ISAS). One of the main uniquenesses of the ASTRO-H satellite is the high sensitivity and imaging capability of the wide energy band from 0.3 keV to 600 keV. The coverage is achieved by combining the four instruments of the SXS, SXI, HXI, and SGD. The other main uniqueness is a spectroscopic capability not only for a point-like source but also for an extended source with high spectral resolution of Δ<em>E</em>~4÷7eV of SXS. Using the unique powers of these instruments, ASTRO-H will address unresolved issues in high-energy astrophysics.

Solar Energetic Electron Events Associated with Hard X-ray Flares 

2021 ◽  
Author(s):  
Wen Wang ◽  
Linghua Wang ◽  
Sam Krucker ◽  
Glenn M. Mason ◽  
Yang Su ◽  
...  
Keyword(s):  
Spectral Index ◽  
Power Law ◽  
Heliocentric Distance ◽  
Energetic Electron ◽  
High Energy ◽  
Thick Target ◽  
The Other ◽  
Ion Acceleration ◽  
X Ray ◽  
Positive Correlation

&lt;p&gt;&lt;span&gt;We investigate 16 solar energetic electron (SEE) events measured by WIND/3DP with a double power-law spectrum and the associated western hard X-ray (HXR) flares measured by RHESSI with good count statistics, from 2002 February to 2016 December. In all 16 cases, the presence of an SEE power-law spectrum extending down to &lt;/span&gt;&lt;span&gt;6&lt;/span&gt;&lt;span&gt;5 keV at 1 AU implies that the SEE source would be high in the corona, at a heliocentric distance of &lt;/span&gt;&lt;span&gt;&gt;&lt;/span&gt;&lt;span&gt;1.3 &lt;/span&gt;&lt;span&gt;solar radii&lt;/span&gt;&lt;span&gt;, while the footpoint or footpoint-like emissions shown in HXR images suggest that the observed HXRs are likely produced mainly by thick target bremsstrahlung processes very low in the corona. &lt;/span&gt;&lt;span&gt;We find that in 8 cases (the other 8 cases), the power-law spectral index of HXR-producing electrons, estimated under the relativistic thick-target bremsstrahlung model, is significantly larger than (similar to) the observed high-energy spectral index of SEEs, with a positive correlation. In addition, the estimated number of SEEs is only &lt;/span&gt;&lt;span&gt;&amp;#8764;&lt;/span&gt;&lt;span&gt;10&lt;/span&gt;&lt;span&gt;-&lt;/span&gt;&lt;span&gt;4 &lt;/span&gt;&lt;span&gt;- &lt;/span&gt;&lt;span&gt;10&lt;/span&gt;&lt;span&gt;-&lt;/span&gt;&lt;span&gt;2 &lt;/span&gt;&lt;span&gt;of the estimated number of HXRproducing electrons at energies above 30 keV, but also with a positive correlation. &lt;/span&gt;&lt;span&gt;These results suggest that in these cases, SEEs are likely formed by upward-traveling electrons from an acceleration source high in the corona, while their downward-traveling counterparts may undergo a secondary acceleration before producing HXRs via thick-target bremsstrahlung processes. In addition, the associated &lt;/span&gt;&lt;span&gt;3&lt;/span&gt;&lt;span&gt;He&lt;/span&gt;&lt;span&gt;=&lt;/span&gt;&lt;span&gt;4&lt;/span&gt;&lt;span&gt;He ratio is positively correlated with &lt;/span&gt;&lt;span&gt;the observed high-energy spectral index of SEEs&lt;/span&gt;&lt;span&gt;, indicating a possible relation of the &lt;/span&gt;&lt;span&gt;3&lt;/span&gt;&lt;span&gt;He ion acceleration with high-energy SEEs&lt;/span&gt;&lt;/p&gt;

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