1.
Earth and The Moon The Home Planet

2.
Earth Evolution <ul><li>First hot and molten </li></ul><ul><li>Heavy material sank toward center </li></ul><ul><ul><li>Differentiation </li></ul></ul><ul><ul><ul><li>Heavy material sinks over time toward the center of the Earth while lighter material rises to the surface. </li></ul></ul></ul><ul><li>Earth cooled from outside in </li></ul><ul><li>Radioactivity continues today to heat interior </li></ul><ul><li>Oldest Earth rocks found on the surface today are about 3.9 billion years old </li></ul><ul><ul><li>this is known from radioactive dating </li></ul></ul><ul><ul><li>therefore, Earth formed at least 3.9 billion years ago </li></ul></ul><ul><ul><ul><li>it actually formed 4.6 billion years ago with the rest of the Solar System </li></ul></ul></ul>

3.
Internal Structure

5.
Revolution

6.
Long Summer Days

7.
Precession <ul><li>There are 2 types of precession </li></ul><ul><li>Earth is obligated 43km larger in equator </li></ul><ul><li>Tidal forces of the sun and the moon </li></ul><ul><li>25700 years period </li></ul>

9.
<ul><li>The force that cause an spinning top to wobble is parallel to its rotation axis at first </li></ul><ul><li>Solar gravity is perpendicular to the Earth’s axis </li></ul><ul><li>The torque is applied to the equatorial bulge </li></ul><ul><li>The torque is always in the same direction, perpendicular the direction of equatorial poles, so it does not change the axial tilt itself. </li></ul>

11.
Precession of Planetary Orbits

12.
Nutation <ul><li>The period of the largest component of the Earth’s nutation is 18.6 years, the same as of the precession of the moons orbital nodes. </li></ul>

13.
Magnetosphere

14.
Aurora

16.
Earth and The Moon Lunar Phases

19.
Calculation: phase=fraction(0.20439731+t*0.03386319269) t = [UT] - [12AM, January 1, 2001], in days

22.
Earth and The Moon Tidal Force

23.
Tidal Force <ul><li>An effect of gravity </li></ul>

24.
Angular Momentum Kepler’s law of equal areas b

25.
h d v |_ v For L to be constant, then the area (a) swept by the planet in a certain length of time ( Δ t) must be always the same.

26.
The high tide is not directly underneath of the moon <ul><li>Friction </li></ul><ul><li>Earth slows down 2X10-9 seconds daily </li></ul><ul><li>Angular momentum’s being transferring to the moon </li></ul><ul><li>The Moon goes farther 38mm each year </li></ul><ul><li>Tidal Acceleration </li></ul>

27.
The Fate of Tidal Effects <ul><li>Earth has already slowed down the moon. </li></ul><ul><li>The period of rotation of the moon = the period of its revolution around the earth. </li></ul><ul><li>The Earth and the moon will finally lock. </li></ul><ul><li>Then the tidal effect of the sun pull the moon closer to the earth (causes the moon reach Roche limit, but 10 milliard years!) </li></ul>

28.
Leap Seconds <ul><li>UT: Based on Earth’s rotation (irregular, tidal effects and melting ice sheets) </li></ul><ul><li>TT: Based on Atomic clocks. </li></ul><ul><li>Δ T = TT-UT </li></ul><ul><li>Leap seconds are being added to Atomic clocks to adjust standard time of day (UTC) close to mean solar time (UT=GMT) (noon @ noon). </li></ul><ul><li>The last leap second added in Dec. 31 2005. </li></ul>

29.
Universal Time – Coordinated Universal Time

30.
<ul><li>Moon Revolution < Earth Rotation so: Tidal acceleration </li></ul><ul><li>What happens for a moon if it orbit faster than the parent body’s rotation? </li></ul>

31.
Earth and The Moon Lunar Impacts

32.
<ul><li>Tycho crater (85km wide, 4.8km deep) </li></ul><ul><li>Central peak </li></ul><ul><li>Craters are named after astronomers </li></ul>

37.
Earth and The Moon Faces of the moon

38.
Near Side (0 degree)

39.
Surface Features <ul><li>Maria - large flat areas resulting from lava flows </li></ul><ul><li>Fourteen (14) named maria, the largest being Mare Imbrium (1100 km diameter) </li></ul><ul><li>Highlands - lighter appearing, elevated areas </li></ul><ul><li>Craters - very old => mostly from meteoritic impact - very old </li></ul><ul><li>Far side surprise </li></ul><ul><li>no major maria => due to asymmetric crust </li></ul><ul><li>almost entirely highlands </li></ul><ul><li>Moon's surface is frozen in time: very little surface erosion </li></ul><ul><li>no wind or running water, to cause erosion </li></ul><ul><li>no plates on surface to cause volcanism or seismic activity </li></ul><ul><li>some erosion from micrometeroids </li></ul><ul><ul><li>cumulative effect of micrometeroids => dust </li></ul></ul>

40.
Far Side (180 degrees)

41.
The Far Side <ul><li>Is shielded form the Earth’s radiation </li></ul><ul><li>Only 2.5% of its surface is Maria </li></ul><ul><li>The crust is 40km thicker on the far side </li></ul><ul><li>Maria are denser than surface mat. </li></ul><ul><li>Moon is oriented in lowest energy configuration (by Earth’s tidal force). </li></ul>

42.
Earth and The Moon Lunar Eclipses

43.
The Red Moon

44.
How?

45.
Compare Distances

48.
<ul><li>Starts: 16 Shahrivar 20:12 </li></ul><ul><li>Ends 17 Shahrivar 00:30 (Tehran Time) </li></ul>

49.
Earth and The Moon Libration

51.
Types of Librations <ul><li>In Latitude: Moon axis is inclined </li></ul><ul><li>In Longitude: The velocity of the moon in its elliptical orbit varies </li></ul><ul><li>Diurnal (daily) </li></ul><ul><li>We can see 59% of the moon due libration </li></ul>

53.
Earth and The Moon Formation

54.
Giant Impact <ul><li>A Mars-size object firstly located in Lagrangian Point L4 or L5 hit the early Earth, just in the best situation </li></ul>

56.
Roche Limit