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The Dynamic Earth and Space Geodesy EATS 1010 3.0 [Fall 2011]

The Dynamic Earth and Space Geodesy EATS 1010 3.0 [Fall 2011]. Instructor: Gary Jarvis, Department of Earth and Space Science & Engineering (ESSE) 117 Petrie Science & Engineering Building jarvis@yorku.ca , 416-736-2100 Ext. 77710

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The Dynamic Earth and Space Geodesy EATS 1010 3.0 [Fall 2011]

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  1. The Dynamic Earth and Space Geodesy EATS 1010 3.0 [Fall 2011] Instructor: Gary Jarvis, Department of Earth and Space Science & Engineering (ESSE) 117 Petrie Science & Engineering Building jarvis@yorku.ca, 416-736-2100 Ext. 77710 Laboratory Coordinator: Terry Du, 77706 terrydu@yorku.ca Text: The Dynamic Earth and Space Geodesy,SC/EATS 1010 3.0(Custom Publication for York University) ESSE office: 102 Petrie Science & Engineering, 416-736-2100 Ext. 55245

  2. The Dynamic Earth and Space Geodesy EATS 1010 3.0 [Fall 2011] Earth as a Planetary Body in Space • Topics • Origin of the Earth Large Scale • Impact Craters • Earth’s Interior • Plate Tectonics • Geomagnetism • Seismology • Space Geodesy & Geomatics • VLBI • GPS • GIS • Remote Sensing Small Scale What is it? How do we measure it?

  3. The Dynamic Earth and Space Geodesy EATS 1010 3.0 [Fall 2011] Course Marking Scheme & Schedule 5 Laboratory Exercises: 20% Sept. 19 – Nov. 25 Mid-Term Test: 30% October 25 Final Exam: 50% December 8 – 22.

  4. EATS 1010 3.0 Lab. Timetable(Fall 2011) Group Day Time Lab 1 Lab 2 Lab 3 Lab 4 Lab 5 Planet Minerals Plate GPS Seismology Earth Tectonics _______________________________________________________________________ 1 M 11:30 Sept. 19 Oct. 3 Oct. 24 Nov. 7 Nov. 21 2 M 2:30 Sept. 19 Oct. 3 Oct. 24 Nov. 7 Nov. 21 3 T 11:30 Sept. 20 Oct. 4 Oct. 25 Nov. 8 Nov. 22 4 T 2:30 Sept. 20 Oct. 4 Oct. 25 Nov. 8 Nov. 22 5 W 11:30 Sept. 21 Oct. 5 Oct. 26 Nov. 9 Nov. 23 6 W 2:30 Sept. 21 Oct. 5 Oct. 26 Nov. 9 Nov. 23 7 R 11:30 Sept. 22 Oct. 6 Oct. 27 Nov. 10 Nov. 24 8 R 2:30 Sept. 22 Oct. 6 Oct. 27 Nov. 10 Nov. 24 9 F 8:30 Sept.23 Oct. 7 Oct. 28 Nov. 11 Nov. 25 10 F 11:30 Sept. 23 Oct. 7 Oct. 28 Nov. 11 Nov. 25

  5. Attendance Lectures - Notes are essential. Text only covers about 50% of material Laboratory Sessions - Mandatory – zero tolerance - Change of lab group only with permission of lab. coordinator. - Lab exercises must be submitted to your group TA. Otherwise no mark.

  6. • • quasar The Visible Universe • • • • • • galaxy galaxy cluster • • • quasar • • galaxy • • • • • • • • • • • • galaxy cluster • • quasar • quasar • Film: Powers of 10

  7. Galaxies Astronomers can see billions of galaxies. Photograph from the Hubble space telescope. The Sun There are 100 billion "Suns" in a galaxy like our own Milky Way Galaxy.

  8. The Milky Way Galaxy as seen edge on from the Solar System

  9. The Milky Way With telescope and time exposure On a clear dark night

  10. Our Solar System Our solar system consists of an average-size star we call the Sun; the planets Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus and Neptune; and the dwarf planet Pluto. It also includes: the satellites of the planets; numerous comets, asteroids, and meteoroids; and the interplanetary medium. Sun Jupiter Saturn Uranus Neptune Mercury Venus Earth Mars Pluto Relative sizes of planets

  11. Formation of the Solar System The “Nebular Hypothesis” • A cloud of interstellar gas/dust, the "solar nebula", including material formed in previous generations of stars, is disturbed (for example, by the shock wave from a nearby supernova).

  12. The collapsing, spinning nebula begins to flatten into a rotating pancake. Formation of the Solar System • 1. Contraction: The cloud starts collapsing under its own gravity.

  13. Formation of the Solar System 2. A Protostarforms in the centre, when the core becomes dense enough; later will become the Sun. • 3. Dust grains stick to each other and sweep their paths, forming larger particles(Planetesimals). • 4. Orbital paths are cleared. 5. The Sun and its planets all spin in the samedirection.

  14. The Sun Within the core of the Sun: temperatures exceed 15,000,000° C and pressure is 340 billion times the atmospheric pressure at Earth's surface. Conditions are so intense that nuclear fusion takes place creating new elements.

  15. Nuclear Fusion in the Sun Four hydrogen nuclei get fused into one helium nucleus, Accompanied by the emission of neutrinos and release of energy: 4 H1 He4 + neutrinos + energy H1 is the nucleus of a hydrogen atom (one proton) He4 is the nucleus of a helium atom (two protons and two neutrons)

  16. Conversion of Mass into Energy The nucleus of the resulting helium atom is about 0.7 percent less massive than the four component protons. During the fusion of hydrogen, approximately 0.7% of the mass of hydrogen is converted into energy. E = mc2

  17. The Solar Wind Fast-moving ions can escape the Sun's gravitational attraction. Moving outward at hundreds of kilometres/second, these positive and negative charges travel to the farthest reaches of the solar system. They are called the solar wind.

  18. Solar Prominences Bursts of solar wind accompany solar prominences (similar to nuclear explosions) which extend millions of km into space. Earth Solar Prominence

  19. Interstellar Distances • The Sun is massive – 99.9% of mass. • The planets are relatively minute: - Jupiter makes up most of the remaining 0.1%. • The next nearest star appears as a point of light. • Similarly, from the nearest star, our Sun would appear as a point of light in the night sky - the planets of our Solar System would not be visible. - similarly planets of other stars are not visible to us, but must exist [detected by wobbles of star due to gravity of orbiting planets]. • Distances between the stars are enormous.

  20. A new unit of distance to measure interstellar space Light Year: The distance light travels in a year, travelling at a speed of 300,000 kilometres per second; 1 light-year is equivalent to 9.46053 x 1012 km ( almost ten trillion km). • The Sun's nearest known stellar neighbour is a star called Proxima Centauri, at a distance of 4.3 light years away (i.e., 4.3 LY). • Some Quasars are more distant than 10 billion LY.

  21. The Solar System is Small Solar System from a Cosmic Perspective Facts: • Average distance from the Sun to Neptune is 4.5 x 109 km • Distance from the Sun to the nearest star is 4.1 x 1013 km (~ 9000 x distance from Sun to Neptune) • The Sun is one of 1022 similar stars. • On a cosmic scale the Solar System is microscopic.

  22. The Solar System is Large Solar System from an Earth Perspective Facts: • The Diameter of Earth is 12.8 x 103 km (DEarth) • The distance from the Sun to Earth is 1.496 x 108 km or about 12,000 x DEarth. • The diameter of Neptune’s orbit is 700,000 x DEarth. • On an Earth scale the Solar System is vast.

  23. A new unit of distance to measure interplanetary space AstronomicalUnit (AU) : The average distance from the Earth to the Sun; 1 AU = 149,597,870 kilometres (~150 million km) 1 LY= 63,240 AU. We can measure distances within the solar system in units of AU’s. e.g., The distance from the Sun to Earth is 1 AU The distance from the Sun to Mars is 1.5 AU The distance from the Sun to Venus is 0.72 AU

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