Seismological Aspects of the 2002 Denali Fault, Alaska, Earthquake

2004 ◽  
Vol 20 (3) ◽  
pp. 555-563 ◽  
Author(s):  
Roger A. Hansen ◽  
Natalia A. Ratchkovski
Keyword(s):  
Energy Release ◽  
High Energy ◽  
Thrust Fault ◽  
Denali Fault ◽  
Rupture Length ◽  
Alaska Earthquake

The M7.9 Denali fault earthquake occurred on 3 November 2002 with an epicenter located 135 km south of Fairbanks and 283 km north of Anchorage. This epicenter is 22–25 km east of the M6.7 Nenana Mountain earthquake that occurred eleven days earlier, October 23, awakening some inhabitants of central Alaska at about 3:30 that morning. Like most earthquakes of its size, the M7.9 earthquake was a complex event. The rupture began with vertical slip along a 40-km segment of the previously unrecognized Susitna Glacier thrust fault, which is connected to the Denali fault. The rupture continued with right-lateral horizontal slip along the main trace of the Denali fault. It eventually split off the Denali fault onto the more southeast-trending Totschunda fault. The total rupture length was 330–340 kilometers, with at least three areas of high slip, or high energy release.

Surface Rupture of the 2002 Denali Fault, Alaska, Earthquake and Comparison with Other Strike-Slip Ruptures

2004 ◽  
Vol 20 (3) ◽  
pp. 565-578 ◽  
Author(s):  
Peter J. Haeussler ◽  
David P. Schwartz ◽  
Timothy E. Dawson ◽  
Heidi D. Stenner ◽  
James J. Lienkaemper ◽  
...  
Keyword(s):  
Thrust Fault ◽  
Strike Slip ◽  
Surface Rupture ◽  
Oil Pipeline ◽  
Denali Fault ◽  
The Past ◽  
Surface Slip ◽  
Lateral Offset ◽  
Large Earthquakes ◽  
Alaska Earthquake

On 3 November 2002, an M7.9 earthquake produced 340 km of surface rupture on the Denali and two related faults in Alaska. The rupture proceeded from west to east and began with a 40-km-long break on a previously unknown thrust fault. Estimates of surface slip on this thrust are 3–6 m. Next came the principal surface break along ∼218 km of the Denali fault. Right-lateral offsets averaged around 5 m and increased eastward to a maximum of nearly 9 m. The fault also ruptured beneath the trans-Alaska oil pipeline, which withstood almost 6 m of lateral offset. Finally, slip turned southeastward onto the Totschunda fault. Right-lateral offsets are up to 3 m, and the surface rupture is about 76 km long. This three-part rupture ranks among the longest strike-slip events of the past two centuries. The earthquake is typical when compared to other large earthquakes on major intracontinental strike-slip faults.

scholarly journals Study on the Fracture Law of Inclined Hard Roof and Surrounding Rock Control of Mining Roadway in Longwall Mining Face

Energies ◽  
2020 ◽  
Vol 13 (20) ◽  
pp. 5344
Author(s):  
Feng Cui ◽  
Shuai Dong ◽  
Xingping Lai ◽  
Jianqiang Chen ◽  
Chong Jia ◽  
...  
Keyword(s):  
Energy Release ◽  
Longwall Mining ◽  
Coal Pillar ◽  
High Energy ◽  
Mechanical Analysis ◽  
Engineering Practice ◽  
Analysis Model ◽  
Hard Roof ◽  
Working Face ◽  
The Stability

In the inclination direction, the fracture law of a longwall face roof is very important for roadway control. Based on the W1123 working face mining of Kuangou coal mine, the roof structure, stress and energy characteristics of W1123 were studied by using mechanical analysis, model testing and engineering practice. The results show that when the width of W1123 is less than 162 m, the roof forms a rock beam structure in the inclined direction, the floor pressure is lower, the energy and frequency of microseismic (MS) events are at a low level, and the stability of the section coal pillar is better. When the width of W1123 increases to 172 m, the roof breaks along the inclined direction, forming a double-hinged structure, the floor pressure is increased, and the frequency and energy of MS events also increases. The roof gathers elastic energy release, and combined with the MS energy release speed it can be considered that the stability of the section coal pillar is better. As the width of W1123 increases to 184 m, the roof in the inclined direction breaks again, forming a multi-hinged stress arch structure, and the floor pressure increases again. MS high-energy events occur frequently, and are not conducive to the stability of the section coal pillar. Finally, through engineering practice we verified the stability of the section coal pillar when the width of W1123 was 172 m, which provides a basis for determining the width of the working face and section coal pillar under similar conditions.

scholarly journals Particle Acceleration in Solar Flares and Coronal Mass Ejections

2000 ◽  
Vol 195 ◽  
pp. 15-25
Author(s):  
R. P. Lin
Keyword(s):  
Particle Acceleration ◽  
Energy Release ◽  
Coronal Mass Ejections ◽  
Solar Flares ◽  
Gamma Ray ◽  
Solar Energetic Particle ◽  
High Energy ◽  
Total Rate ◽  
Solar Energetic Particle Events ◽  
High Energy Particles

The Sun accelerates ions up to tens of GeV and electrons up to 100s of MeV in solar flares and coronal mass ejections. The energy in the accelerated tens-of-keV electrons and possibly ~1 MeV ions constitutes a significant fraction of the total energy released in a flare, implying that the particle acceleration and flare energy release mechanisms are intimately related. The total rate of energy release in transients from flares down to microflares/nanoflares may be significant for heating the active solar corona.Shock waves driven by fast CMEs appear to accelerate the high-energy particles in large solar energetic particle events detected at 1 AU. Smaller SEP events are dominated by ~1 to tens-of-keV electrons, with low fluxes of up to a few MeV/nucleon ions, typically enriched in 3He. The acceleration in gamma-ray flares appears to resemble that in these small electron-3He SEP events.

scholarly journals Effect of C–O Bonding on the Stability and Energetics of High-Energy Nitrogen-Carbon Molecules N10C2 and N16C2

2014 ◽  
Vol 2014 ◽  
pp. 1-7
Author(s):  
Douglas L. Strout
Keyword(s):  
Energy Release ◽  
High Energy ◽  
Energy Materials ◽  
Complex Molecules ◽  
High Energy Materials ◽  
Rapid Decomposition ◽  
The Subject ◽  
Carbon Molecules ◽  
The Stability ◽  
Thermodynamic Energy

Molecules consisting of nitrogen have been the subject of much attention due to their potential as high-energy materials. Complex molecules consisting entirely of nitrogen can be subject to rapid decomposition, and therefore other atoms are incorporated into the structure to enhance stability. Previous studies have explored the incorporation of carbon atoms into otherwise all-nitrogen cages molecules. The current study involves two such cages, N10C2 and N16C2, whose structures are derived from N12 and N18, respectively. The N10C2 and N16C2 cages in this study are modified by bonding groups O3 and CO3 to determine the effect on the relative energies between the isomers and on the thermodynamic energy release properties. Energetic trends for N10C2 and N16C2 are calculated and discussed.

The Energy Release to Static Gas From a 12-Joule High Energy Ignition System

1977 ◽  
Author(s):  
J. Odgers ◽  
A. Coban
Keyword(s):  
Carbon Dioxide ◽  
Energy Source ◽  
Ionization Potential ◽  
Energy Release ◽  
High Energy ◽  
Scattered Data ◽  
Statistical Nature ◽  
Ignition System

Details are given of a calorimetric-bomb technique used to determine the energy released to the gas, from a spark derived from a high-energy source (∼12J). The statistical nature of the energy release is commented upon, and the number of repeat tests required to obtain a valid mean is discussed. Scattered data from other sources are cited, together with their relevance to the present tests. Measurements of energy are given for the single plug which was subjected to exhaustive testing over a range of pressures from 1.0 kPa to 2500 kPa, and which was repeated for various gases, namely — air, oxygen, nitrogen, carbon dioxide, helium and argon. The results of these tests may be correlated in terms of the pressure and the ionization potential of the gas.

scholarly journals Generation of Magnetic Fields in Accreting Systems as a Basis of Nonthermal Mode of Energy Release

1993 ◽  
Vol 157 ◽  
pp. 197-201
Author(s):  
L.A. Pustil'Nik ◽  
N.R. Ikhsanov
Keyword(s):  
Magnetic Field ◽  
Black Hole ◽  
Magnetic Fields ◽  
Energy Release ◽  
Polar Region ◽  
High Energy ◽  
Ultra High Energy ◽  
The Magnetic Field

Generation of the magnetic field during procces of disc accretion onto black hole or magnetize neutrin star may form current structures in a polar region. The instability and disruption of this currents must lead to effective acceleration of the particles to ultra high energy as it observe by GRO and UHE-astronomy experiments.

Large rock avalanches triggered by the M 7.9 Denali Fault, Alaska, earthquake of 3 November 2002

2006 ◽  
Vol 83 (1-3) ◽  
pp. 144-160 ◽  
Author(s):  
Randall W. Jibson ◽  
Edwin L. Harp ◽  
William Schulz ◽  
David K. Keefer
Keyword(s):  
Denali Fault ◽  
Rock Avalanches ◽  
Alaska Earthquake

High energy release boron-based material with oxygen vacancies promoting combustion

2021 ◽  
pp. 133027
Author(s):  
Hui-xin Wang ◽  
Hui Ren ◽  
Liu Yin ◽  
Ya-ru Li ◽  
Xin-zhou Wu
Keyword(s):  
Energy Release ◽  
Oxygen Vacancies ◽  
High Energy

Energetic Al/Fe2O3/PVDF composites for high energy release: Importance of polymer binder and interface

2016 ◽  
Vol 24 (10) ◽  
pp. 909-914 ◽  
Author(s):  
Jae Hun Lee ◽  
Sang Jin Kim ◽  
Jung Soo Park ◽  
Jong Hak Kim
Keyword(s):  
Energy Release ◽  
High Energy ◽  
Polymer Binder

scholarly journals On the Onset Time of Several SPE/GLE Events: Indications from High-Energy Gamma-Ray and Neutron Measurements by CORONAS-F

2013 ◽  
Vol 2013 ◽  
pp. 1-15 ◽  
Author(s):  
Viktoria Kurt ◽  
Karel Kudela ◽  
Boris Yushkov ◽  
Vladimir Galkin
Keyword(s):  
Energy Release ◽  
Gamma Ray ◽  
Time Lag ◽  
Onset Time ◽  
High Energy ◽  
Propagation Time ◽  
Pion Decay ◽  
Time Behavior ◽  
High Energy Gamma ◽  
Energy Gamma

We analyzed the high-energy gamma and neutron emissions observed by the SONG instrument onboard the CORONAS-F satellite during August 25, 2001, October 28, 2003, November 4, 2003, and January 20, 2005 solar flares. These flares produced neutrons and/or protons recorded near Earth. The SONG response was consistent with detection of the pion-decay gamma emission and neutrons in these events. We supposed that a time profile of the soft X-ray derivative was a good proxy of time behavior of the flare energy release. Then we showed that time intervals of the maximum both of energy release and pion-decay-emission coincided well. We determined the onset time of GLEs 65, 69 on the basis of neutron monitor data using the superposed epoch method. The time of high-energy proton onset on November 4, 2003 was found from the GOES data. The time delay between the high-energy gamma ray observation and the high-energy protons onset time was <5 minutes. This time lag corresponds to the least possible proton propagation time. So, we conclude that in these events both protons interacted in the solar atmosphere and the first protons which arrived to Earth, belonged to one and the same population of the accelerated particles.

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