scholarly journals Observations of runup and energy flux on a low-slope beach with high-energy, long-period ocean swell

2015 ◽  
Vol 42 (22) ◽  
pp. 9933-9941 ◽  
Author(s):  
Julia W. Fiedler ◽  
Katherine L. Brodie ◽  
Jesse E. McNinch ◽  
Robert T. Guza
Keyword(s):  
Energy Flux ◽  
High Energy ◽  
Long Period ◽  
Slope Beach

Long Period Gratings in Multimode Fiber Fabricated with High-Energy Ion Implantation

2003 ◽  
Vol 22 (4) ◽  
pp. 225-237
Author(s):  
K. J. GRANT ◽  
ROBERTS A. ◽  
D. N. JAMIESON ◽  
B. ROUT ◽  
C. CHER
Keyword(s):  
Ion Implantation ◽  
High Energy ◽  
Multimode Fiber ◽  
Long Period ◽  
Long Period Gratings

Long Period Gratings in Multimode Fiber Fabricated with High-Energy Ion Implantation

2003 ◽  
Vol 22 (4) ◽  
pp. 225-237 ◽  
Author(s):  
GRANT ◽  
A. ROBERTS
Keyword(s):  
Ion Implantation ◽  
High Energy ◽  
Multimode Fiber ◽  
Long Period ◽  
Long Period Gratings

scholarly journals Characterization of the HD 219134 multiplanet system I. Observations of stellar magnetism, wind, and high-energy flux★

2018 ◽  
Vol 481 (4) ◽  
pp. 5286-5295 ◽  
Author(s):  
C P Folsom ◽  
L Fossati ◽  
B E Wood ◽  
A G Sreejith ◽  
P E Cubillos ◽  
...  
Keyword(s):  
Energy Flux ◽  
High Energy

scholarly journals CHARACTERISTICS OF SHINGLE BEACHES WITH REFERENCE TO CHRISTCHURCH BAY, S. ENGLAND

1988 ◽  
Vol 1 (21) ◽  
pp. 142 ◽  
Author(s):  
Robert Nicholls ◽  
Norman Webber
Keyword(s):  
High Energy ◽  
Sand Fraction ◽  
Distinctive Character ◽  
Long Period ◽  
Seepage Characteristics ◽  
Run Up ◽  
The Stability ◽  
Natural Laboratory

The rapid recession of the shingle bank of Hurst Beach (up to 3.5m/yr) makes it an excellent natural laboratory for the study of the factors which influence the stability of shingle beaches. Studies have included: the significance of long period, high energy, swell waves - the classification and quantification of overwash processes - run-up and seepage characteristics - the effect of settlement of the underlying strata - and the implications for practices in shingle nourishment. The studies have revealed the distinctive character of shingle beaches as compared with the more fully researched sand beaches. More detailed research on shingle beaches is justified particularly in relation to (i) the run-up characteristics including its interaction with swash cusps and (ii) the influence of the subsidiary sand fraction on the beach characteristics.

Pulsed X-Ray Annealing of Arsenic-Implanted Silicon

1981 ◽  
Vol 4 ◽  
Author(s):  
T. W. Sigmon ◽  
D. E. Osias ◽  
R. L. Schneider ◽  
C. Gilman ◽  
G. Dahlbacka
Keyword(s):  
Energy Density ◽  
Structural Properties ◽  
Energy Flux ◽  
High Energy ◽  
Wafer Surface ◽  
X Rays ◽  
Density Range ◽  
X Ray ◽  
Large Numbers ◽  
Unique Capability

ABSTRACTIn this paper we report experiments on annealing of arsenic-implanted silicon using a pulsed imploding-plasma X-ray source. Silicon wafers of <100> orientation were implanted with arsenic ions at 50 keV to a dose of 3.5 ∼ 1015 cm−2 and exposed to a single 50 ns pulse of X-rays in the energy density range of 0.15 to 0.55 J/cm2 The characteristic X-ray absorptiog coeificient in silicon for these experiments was 1.6 ∼ 10 cm−1, resulting in most of the energy being absorbed in the first 100 nm of the wafer surface.For wafers annealed in the energy density range of 0.3 to 0.4 J/cm2 backscattering and channeling measurements show recovery of the crystallinity of the damaged layer with incorporation of about 86% of the implanted arsenic onto substitutional lattice positions. Evidence of redistribution and flattening of the arsenic profile in the annealed wafer was observed in the backscattering data and confirmed by SIMS profiling. Detailed results on the electrical and structural properties of these annealed layers will be presented. High energy pulsed X-ray sources offer the unique capability of simultaneously exposing large numbers of wafers to an extremely uniform energy flux at much higher efficiencies than conventional lasers.

scholarly journals CAPACITY OF INLET OUTER EARS TO STORE SAND

1976 ◽  
Vol 1 (15) ◽  
pp. 111 ◽  
Author(s):  
Todd L. Walton ◽  
William D. Adams
Keyword(s):  
Energy Flux ◽  
High Energy ◽  
Wave Activity ◽  
Wave Action ◽  
Low Energy ◽  
Tidal Prism ◽  
Governing Parameter ◽  
High Wave ◽  
Upper Limit ◽  
Storage Volume

Inlets act as large sand sinks for sand derived from adjacent beaches. An attempt to quantify the amount of sand in an outer bar is made with the major governing parameter of inlet hydraulics, tidal prism. In areas of high wave activity there appears to be a well defined limiting relationship to the amount of sand stored in the offshore bar as a function of tidal prism. In areas where inlets are exposed to lower wave activity, more scatter is noted in this correlation. Relationships for estimating the equilibrium storage volume of sand in the outer bar/shoal of newly cut inlets on highly exposed, moderately exposed, and mildly exposed coasts (where degree of exposure relates to wave action offshore) are proposed for use in estimating quantities of sand which will eventually be lost to adjacent beaches. A conclusion of the study is that more sand is stored in the outer bar of a low energy coast than in the outer bar of a high energy coast. An upper limit to outer bar storage in low energy zones may be a function of additional parameters other than tidal prism such as longshore energy flux at the inlet site and inlet history.

scholarly journals The Termination Shock in a Striped Pulsar Wind

2004 ◽  
Vol 218 ◽  
pp. 167-170
Author(s):  
Yury Lyubarsky
Keyword(s):  
Energy Flux ◽  
High Energy ◽  
Magnetic Polarity ◽  
Termination Shock ◽  
Fermi Acceleration ◽  
High Energy Tail ◽  
Total Energy Flux ◽  
Equatorial Belt ◽  
Pulsar Wind ◽  
Downstream Flow

Toroidal stripes of opposite magnetic polarity are formed in the equatorial belt of the wind emanating from an obliquely rotating pulsar magnetosphere. Such a striped wind transfers most of its spindown energy because the angular distribution of the energy flux in the pulsar wind is maximum at the equator. The alternating field annihilates either in the pulsar wind or at the termination shock so that the flow in the equatorial belt downstream of the termination shock is weakly magnetized. At high latitudes, the magnetization of the flow is higher than in the equatorial belt whereas the total energy flux is smaller. At such a distribution of the energy flux and magnetization, the downstream flow separates into an equatorial disk and a magnetically collimated polar jet. Particle acceleration at the termination shock in a striped wind is discussed. It is argued that the radio emitting electrons are accelerated by driven reconnection of the alternating field at the shock whereas the Fermi acceleration of electrons preaccelerated in the reconnection process results in a high energy tail responsible for the X- and γ-ray emission.

A RHEED study of Cu3Au (110) surface

1992 ◽  
Vol 50 (2) ◽  
pp. 1460-1461
Author(s):  
Yi Huang ◽  
John M. Cowley
Keyword(s):  
Electron Diffraction ◽  
Auger Electron Spectroscopy ◽  
Electron Spectroscopy ◽  
Auger Electron ◽  
Room Temperature ◽  
High Energy ◽  
High Energy Electron ◽  
Ion Scattering ◽  
Long Period ◽  
The Ideal

In recent years the Cu3Au (110) surface has been studied by many authors to reveal its ordering structure and order-disorder transition phenomena. A 2×1 structure which corresponds to an ideal truncation of the ordered bulk crystal and a 4×1 reconstructed structure have been observed. Using ion scattering methods, McRae et al have determined the Au fractions in the first and the second layer at room temperature, which deviate from the ideal bulk value and indicate the segregation of Au to the surface. But the question how the atoms are rearranged in the 4×1 structure and why some of the Au stays in the second layer have not been answered. Another important question about Cu3Au (110) surface is whether the long period ordering structure (LPS) exists on the surface. In present work the Cu3Au (precise composition Cu71.7Au28.3) (110) surface is studied with Auger electron Spectroscopy (AES) and Reflection High Energy Electron Diffraction (RHEED) which have not been used to study the Cu3Au surface before.

Сomparison of ion pressure variations derived from Cluster/CODIF and the combined Cluster/CODIF&RAPID data during prolonged dipolarizations in the near Earth magnetotail

2020 ◽  
Author(s):  
Andrey Malykhin ◽  
Elena Grigorenko ◽  
Elena Kronberg ◽  
Patrick Daly
Keyword(s):  
Energy Range ◽  
Energy Flux ◽  
Total Pressure ◽  
High Energy ◽  
Plasma Pressure ◽  
Energy Threshold ◽  
Superposed Epoch Analysis ◽  
Flux Increase ◽  
Epoch Analysis ◽  
Thermal Part

&lt;p&gt;Usually, for the plasma pressure estimation in the plasma sheet&amp;#160; ion observations in the energy range up to ~40 keV are used. However, the thermal part of the distribution function can pass beyond the high energy threshold of an instrument during active events like dipolarizations. In such cases the entire ion population is not measured and the ion pressure can be underestimated. We study this problem by using Cluster mission observations provided&amp;#160; by two instruments: thermal plasma instrument - CODIF (up to 38 keV) and suprathermal instrument - RAPID (from 40 up to 1500 keV). We analyzed 11 dipolarization events and showed that in all events the maximum of ion energy flux was shifted to high energy threshold of CODIF instrument. Simultaneously, the energy flux increase in suprathermal energy range was observed by RAPID. For H&lt;sup&gt;+&lt;/sup&gt; and O&lt;sup&gt;+&lt;/sup&gt; ion components we calculate the pressure of suprathermal population and showed that the total pressure estimated by using both CODIF and RAPID instruments at some intervals exceeds the pressure estimated only from CODIF data up to 5 times. The superposed epoch analysis applied to 11 dipolarization events from our data base showed that the total pressure of H&lt;sup&gt;+&lt;/sup&gt; and O&lt;sup&gt;+&lt;/sup&gt; ion components can be in 2-5 times underestimated in the course of dipolarization.&lt;/p&gt;

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