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TOPICS 3&4 ASTRONOMY
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All the matter in the universe, is thought to be contained in an area no larger than a grain of sand This area was under extreme pressure and measured an infinite density The matter exploded and traveled outward at an extreme rate This matter is still expanding and moving outward after billions of years This theory explains the origin of the universe
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Rotation-
A. Earth’s 1. Direction of Rotation:
Counterclockwise (CCW)
West to East (Left Right)
2. Rate of Rotation
a. 360 degrees
b. 24 hours
3. RATE= 15º/ hour
The movement or turning of a celestial body on its axis (spinning)
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What Happens If Earth’s Rotation slows down Video 2:53
The Earth and Its Motions
The rotation of the Earth causes day & night.
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Effects of Earth’s Rotation
The Apparent Motions of stars Star trail photographs looking North, South,
East, and West Try to identify the star trail photo and the
direction you would be facing
*15°/ hour*
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Effects of Earth’s Rotation
Apparent Motions of the Suna. Earth rotates from _______ to _______
b. Sun appears to move in an arc from ____________ to ____________ West
EastWest
East
*15°/ hour*
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Evidence of Rotation Pendulum- the Foucault Pendulum is a device
that proves (evidence) the Earth rotates on its axis
Coriolis Effect- is the deflection of planetary winds and ocean currents. In the Northern Hemisphere winds deflect to the right & to the left in the Southern Hemisphere
Classzone Animation
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Revolution-Revolution-
• A.A. Rate of RevolutionRate of Revolution 1. 1. 22. .
Earth revolves around the sunEarth revolves around the sun
1º/day1º/day
The orbiting of one celestial body around another celestial body
360 degrees
365 days
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Diagram of Earth’s RevolutionDiagram of Earth’s RevolutionLabel positions A-DLabel positions A-D
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Evidence of Earth’s Revolution1. Annual, cyclic changing of the
constellations seen at night
2. Seasonal Changes- the seasons
change in a cyclic pattern every
year
winter
spring
summer
autumn
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Evidence of Earth’s Revolution3. Annual, cyclic variations of the length
of daylight hours
Animate
http://www.learner.org/jnorth/images/graphics/mclass/SunlightAnimation_Year.gif
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Evidence of Earth’s Revolution4. Parallax- the slight changing of the position of
distant stars
Parsec- A unit of astronomical length based on the distance from Earth at which stellar parallax is one second of arc and equal to 3.258 light-years, 3.086 × 1013 kilometers, or 1.918 × 1013 miles.
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TERRESTRIAL PLANETS
Images: Lunar and Planetary Laboratory: http://solarsystem.nasa.gov/multimedia/display.cfm?IM_ID=178
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Rocky Dense Metal cores (iron) few moons AKA “inner planets”
Close to Sun small slow rotation fast revolution solid surfaces
Jovian Planets
Large (big diameters)
Massive
Gases and liquids
No solid surface
All have rings
Rotate rapidly
Slow revolution
Many moonsImage: Lunar and Planetary Laboratory: http://solarsystem.nasa.gov/multimedia/display.cfm?IM_ID=178
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Diagram of Earth’s Revolution11. Label positions A-D
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Season & Season & Approximate Approximate DateDate
Latitude Latitude of Sun’s of Sun’s Direct Direct RaysRays
Direction Direction of of Sunrise Sunrise & Sunset& Sunset
Altitude Altitude of the of the Noon Noon SunSun
Period of Period of DaylightDaylight
June 21June 21stst
SummerSummer SolsticeSolstice
23.5° 23.5° NorthNorth
North of North of East & East & North of North of WestWest
≈ ≈ 75°75° 15 Hours15 Hours
September 23rd
Autumnal Equinox (Fall)
0° Equator
Due East & Due West
≈ 50° 12 Hours
December 21December 21stst
WinterWinter Solstice Solstice23.5° 23.5° SouthSouth
South of South of East & East & South of South of WestWest
≈ ≈ 25°25° 9 Hours9 Hours
March 21March 21stst
VernalVernal Equinox Equinox (Spring)(Spring)
0° 0° EquatorEquator
Due East Due East & Due & Due WestWest
≈ ≈ 50°50° 12 Hours12 Hours
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Celestial Sphere1. Label horizon & zenith
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Celestial Sphere2. Blue= 12/21, Green= 3/21 &
9/23, Red=6/21
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Celestial Sphere3. 42°N b/c that’s the altitude
of Polaris
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Celestial Sphere4. South
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Kepler’s Laws of Planetary Motion
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Kepler’s 1st LawTitled the: Ellipse LawStates each planet moves around the
Sun in an ellipse with the Sun located at one focus
Focus Focus
Sun Sun
Planet
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Kepler’s 1st Law: Definitions• Ellipse: A closed curve around two
fixed points, called foci; shaped like an oval or flattened circle
• Foci: Two fixed points within the ellipse – Think of the ellipse as a smiley face with
the two eyes being the fociFocus Focus
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Kepler’s 1st Law
Label the parts of the Ellipse:
Focus Focus
Major Axis:
The longest diameter (axis) of an ellipse, running through the center and foci.
Minor Axis
Orbit:
The path of an object revolving around another object; such as the Earth around the sun.
Sun Sun
Planet
D= Origin
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Kepler’s 1st Law: Definitions• Eccentricity: is a numerical value
used to describe the degree of flatness or “ovalness” of an ellipse – How out of round the shape is – *Eccentricity of a perfect circle= 0
Circle= 0
Comet Straight line= 1
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Calculating eccentricity of an ellipse:
Formula: (e) eccentricity = (d) distance between foci (L) length of major axis
length of major axis
When the distance between foci get larger what happens to the ellipse?
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d. Relationship:As the distance between foci increases, the shape of the ellipse becomes more elliptical or oval
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ESRT Page 15
Which planet has the least perfectly circular orbit?
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Which planet has the most perfectly circular orbit?
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Kepler’s 2nd Law• Titled: Equal Time, Equal AreaStates as a planet revolves around the
Sun a straight line joining the center of the planet and the center of the Sun, the planets sweeps out equal areas in space in equal intervals of time
Eccentricity Website
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Kepler’s 2nd Law• Essentially what Kepler
discovered was the planets change speed during their orbit around the Sun
http://astro.unl.edu/
naap/pos/animations/kepler.swf
Glencoe
Another
Interactive Animation #2
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Increasing speed
PerihelionJan. 4thMax. speed
AphelionJuly 4thMin speed
Decreasing speed
Max. Gravitational Attraction
MAX Apparent DiameterMin. Gravity
Min diameterHINT: Study one know the other by default
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Kepler’s 3rd Law• Titled The Harmonic Law
States a planet’s orbital period (P) squared is proportional to its average distance from the sun (au) cubed:
What does it mean?
The further a planet is to the sun, the longer it takes to revolve around the Sun
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What are Kepler’s 3 Laws of Planetary Motion?
1. The Ellipse Law: Each planet moves around the Sun in an ellipse with the Sun at one focus
2. Equal areas in space in equal intervals of time (Planets change speed in orbit: Closer to sun= faster)
3. Period squared (2)= Distance cubed (3)(faster period of revolution when closer to sun)
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Increasing speedPerihelion
Jan. 4thMax. speed
AphelionJuly 4thMin speed
Decreasing speed
Min Gravitational Attraction
Min Apparent DiameterMax Gravity
Max diameterHINT: Study one know the other by default
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Increasing speed
Decreasing speed
5. THE SUN6. Heliocentric
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Earth’s MoonPAGE 11
Earth’s Moon PAGE 11
New Moon
Waning Gibbous
Full Moon
Waxing Gibbous
First Quarter
Waxing Crescent
Third Quarter
Waning Crescent
Lunar Phases- Seen from Earth
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Earth’s Moon2. 27.3 (ESRT page 15)
3. 27.3 (synchronous motion- this is why we only see one side of the moon)
4. 29.5 days
5. b/c the moon revolves around Earth
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Lunar Eclipse• Moon goes into Earth’s Shadow
• Can only happen in the Full Moon Phase
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Solar Eclipse• Moon blocks out sunlight from
reaching Earth- day turns to night• New Moon Phase
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