Meteorite Classification and Trajectory Modeling

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Meteorite Classification and Trajectory Modeling

  1. 1. Meteorite Classification and trajectory modeling<br />Jessie Miller<br />Ohio Wesleyan University<br />Department of Physics and Astronomy<br />Faculty Advisors: <br />Barbara Andereck and Karen Fryer<br />
  2. 2. Three Main Types of Meteorites<br />Stony<br />Iron<br />Stony Iron<br />
  3. 3. Stony Meteorites<br />Chondrites: <br /><ul><li>most abundant meteorites found on Earth
  4. 4. chemically primitive (low metallicities )
  5. 5. chondrules</li></ul>Achondrites<br /><ul><li>Chondrites that have been changed slightly by melting and recrystallization
  6. 6. contain igneous inclusions</li></li></ul><li>Iron Meteorites<br /><ul><li>pieces of the differentiated cores of asteroids
  7. 7. can be designated into three major categories and other smaller categories through studying their Widmanstatten etching patterns</li></li></ul><li>Stony Iron Meteorites<br />Have characteristics of both stony and iron meteorites<br />
  8. 8. Origin of Meteorites<br />
  9. 9. Thin Section Microscopy<br />Logitech.uk<br />EOS<br />Molecular Expressions<br />
  10. 10. Properties in Plane-Polarized Light<br />Crystal habit <br />Cleavage<br />Relief<br />Microlab Northwest<br />UND<br />
  11. 11. Extinction<br />Isotropic Minerals<br />Anisotropic Minerals<br />Speed of light through mineral is same in all directions<br />Light travels through mineral unaffected<br />All light is absorbed by analyzer<br />Speed of light through mineral is dependent on direction<br />Light is doubly refracted (split into two rays- slow ray and fast ray)<br />Some light passes through analyzer for most orientations<br />Sorrel.humboldt.edu<br />Webassign.net<br />
  12. 12. Interference Colors<br />Olympus<br />Note: tsis time for slow ray to reach analyzer, d is thickness of thin section, V is speed of light in given mediums, n is index of refraction, Δ is retardation<br />
  13. 13. DT 12-8 – H4 Chondrite<br />
  14. 14. NWA 5546 – CV3 Chondrite<br />
  15. 15. Modeling – Equations of Motion<br /> mm*xm''[t]=((xe[t]-xm[t]) G mm me)/((xe[t]-xm[t])^2+(ye[t]-ym[t])^2)^(3/2)+((xs[t]-xm[t]) G ms mm)/((xs[t]-xm[t])^2+(ys[t]-ym[t])^2)^(3/2)<br /> mm*ym''[t]=((ye[t]-ym[t]) G mm me)/((xe[t]-xm[t])^2+(ye[t]-ym[t])^2)^(3/2)+((ys[t]-ym[t]) G ms mm)/((xs[t]-xm[t])^2+(ys[t]-ym[t])^2)^(3/2)<br />
  16. 16. Modeling – Initial Conditions<br />initial positions and velocities of the Earth and the meteoroid relative to the center of mass of the system were given<br />both bodies assumed to start at periapsis (position in orbit closest to central body) on the x-axis, resulting in initial y positions of zero<br />initial x velocities are zero<br />initial y velocities found using the equation<br /> where M is the mass of the body being directly orbited (mefor the meteoroid and ms for Earth).<br />
  17. 17. Orbital Plots<br />
  18. 18. Future Work<br />Assign Earth finite size<br />Time-step through orbits to <br /> locate time of possible impact <br />Based on the incoming velocity and angle of the meteoroid, it may either collide with Earth or be deflected<br />Determine the percent of meteoroids that collide with Earth versus the percent that are deflected<br />In this final form, the program could be used to detect imminent meteorite impacts.<br />

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