221 |
Neutron inelastic scattering studies of the Ising system FeCO(subscript 3)Wrege, Douglas Ewart 12 1900 (has links)
No description available.
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222 |
Thermal-neutron multiple scattering : critical double scatteringHolm, William Alexander 08 1900 (has links)
No description available.
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223 |
Characteristic scattering of low-energy electrons from partially disordered copper and nickel crystalsJordan, Leland Kay 08 1900 (has links)
No description available.
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224 |
Scattering of he+ ions by noble gases at high energiesTaylor, George Ormsbee 12 1900 (has links)
No description available.
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225 |
Scattering at large momentum and energy transfer: application to neutron scattering on liquid heliumRodriguez, Leonard Julius 08 1900 (has links)
No description available.
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226 |
Temperature dependence of the magnetic excitations in iron and nickelLynn, Jeffrey Whidden 05 1900 (has links)
No description available.
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227 |
Scattering of low-energy electrons from the tungsten (110) surfaceTharp, Lester Neal 08 1900 (has links)
No description available.
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228 |
Correlation length and compressibility for polar fluids near their critical pointsPatterson, Edward Matthew 05 1900 (has links)
No description available.
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229 |
Simulations of planet migration driven by the scattering of smaller bodiesKirsh, David Robert 17 September 2007 (has links)
Planet migration is an important part of the formation of planetary systems, both in the Solar system and in extrasolar systems. When a planet scatters nearby comet- and asteroid-size bodies called planetesimals, a significant angular momentum exchange can occur, enough to cause a rapid, self-sustained migration (change of semi-major axis) of the planet. This migration has been studied for the particular case of the four outer planets of the Solar System, but is not well understood in general.
This thesis used the Miranda computer simulation code to perform a broad parameter-space survey of the physical variables that determine the migration of a single planet in a planetesimal disk. A simple model presented within matched well with the dependencies of the migration rate for low-mass planets in relatively high-mass disks. When the planet's mass exceeded that of the planetesimals within a few Hill radii, the migration rate decreased strongly with planet mass. Other trends were identified with the root-mean-squared eccentricity of the planetesimal disk, the mass of the particles dragged by the planet in the corotation region, and the index of the surface density power law. The issue of resolution was also addressed, and it was shown that many previous works in this field may have suffered from being under-resolved.
The trends were discussed in the context of an analysis of the scattering process itself, which was performed using a large simulation of massless planetesimals. In particular, a bias in scattering timescales on either side of the planet's orbit leads to a very strong tendency for the planet to migrate inwards, instead of outwards.
The results of this work show that planet migration driven by planetesimal scattering should be a widespread phenomenon, especially for low-mass planets such as still-forming protoplanets. The simple model provided here, augmented by many more subtle effects, will prove essential to any future work in this underestimated field. / Thesis (Master, Physics, Engineering Physics and Astronomy) -- Queen's University, 2007-09-09 14:28:46.501
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230 |
Coulombic resonances in a zero-gap semiconductor : a variational approach to a problem of resonance in scatteringJoos, Béla. January 1978 (has links)
No description available.
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