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Midterm 1Review
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What is the name of the galaxy cluster containing our own galaxy?
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1. The Solar System
2. The Milky Way
3. The Solar Group
4. The Local Group
5. The Local Cluster1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20
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Distance to the nearest large galaxies:Distance to the nearest large galaxies: several million light yearsseveral million light years
The Local Group of GalaxiesGalaxies usually don’t exist alone, but inGalaxies usually don’t exist alone, but in clusters of galaxiesclusters of galaxies
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Clusters of galaxies are grouped intoClusters of galaxies are grouped into superclusterssuperclusters..Superclusters formSuperclusters form filamentsfilaments and and wallswalls around around voidsvoids..
The Universe on Very Large Scales
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The Astronomical Unit (AU) is defined as
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1. The time it takes for the moon to orbit once around the Earth
2. The distance between the Earth and the moon
3. The distance between the Earth and the sun
4. The diameter of the Earth5. The size of the solar
system
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9.5*109 equals
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1. 10995
2. 95,000,000,000
3. 9,500,000,000
4. 950,000,000
5. 951,000,000,000
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Orbits in the Solar System
Plu
toN
eptu
neUra
nus
Saturn
Jupi
terM
ars
(Distances and times reproduced to scale)
Asteroids
Comets
~ 50 AU
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Which planet’s orbit is the most highly inclined against the ecliptic?
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1. Mercury
2. Venus
3. Jupiter
4. Uranus
5. Pluto
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Retrograde rotation Tipped over by more than 900
Mercury and Pluto: Unusually highly inclined orbits
Planetary Orbits and Rotation
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Over the course of the night, stars are rising in the … and setting in the …
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1. North / South
2. East / West
3. South / North
4. West / East
5. East / East
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Apparent Motion of the Celestial Sphere
Geo
grap
hic
Latit
ude l
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Which of the following values of visual magnitudes seem correct to you?
1. A
2. B
3. C
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Object Magnitude
A B C
Sun 26.5 -26.5 -26.5
Full Moon 12.5 -12.5 -12.5
Venus 4 -4 5
Sirius 1.4 -1.4 0
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The magnitude scale system can be extended towards negative numbers (very bright) and
numbers > 6 (faint objects):
Sirius (brightest star in the sky): mv = -1.42
Full moon: mv = -12.5
Sun: mv = -26.5
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Which of the following is the longest time?
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1. The Earth’s orbital period2. The moon’s sidereal
orbital period3. One precession cycle4. The moon’s synodic
orbital period5. The Saros cycle
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Precession (I)
Gravity is pulling on a slanted top. => Wobbling around the vertical.
The Sun’s gravity is doing the same to the Earth.
The resulting “wobbling” of the Earth’s axis of rotation around the vertical
w.r.t. the Ecliptic takes about 26,000 years and is called precession.
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The Phases of the Moon
• The moon’s synodic period (to reach the
same position relative to the sun) is 29.53 days (~ 1 month).
Fixed direction in space
Earth
Moon
Earth orbits around Sun => Direction toward Sun changes!
29.53 days
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Conditions for Eclipses (II)
Eclipses occur in a cyclic pattern.
→ Saros cycle: 18 years, 11 days, 8 hours
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Spring and Neap Tides
The Sun is also producing tidal effects, about half as strong as the Moon.
• Near Full and New Moon, those two effects add up to cause spring tides
• Near first and third quarter, the two effects work at a right angle w.r.t. each other, causing neap tides.
Spring tides
Neap tides
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A Total Lunar Eclipse (II)
A total lunar eclipse can last up to 1 hour
and 40 min.
During a total eclipse, the moon has a faint, red
glow, reflecting sun light scattered in
the Earth’s atmosphere.
There are ~ 1 – 2 lunar eclipses per year.
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An annular solar eclipse can occur when …
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1. The Earth is near apogee and the moon is near perihelion.
2. The Earth is near aphelion and the moon is near perigee.
3. The Earth is near perihelion and the moon is near apogee.
4. The Earth is near perigee and the moon is near aphelion.
5. Both the Earth and the Moon are near perihelion.
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Earth’s and Moon’s orbits are slightly elliptical:
Sun
Earth
Moon
(Eccentricities greatly exaggerated!)
Perihelion = position closest to the sun (January)
Aphelion = position furthest away from the sun (July)
Perigee = position closest to Earth
Apogee = position furthest away from Earth
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Kepler’s 2nd Law states that …
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1. The acceleration of a body is proportional to the force exerted on it, divided by the mass of the body.
2. To every force there is an equal and opposite force balancing it.
3. The planets are moving around the sun on ellipses with the sun in one focus.
4. The planets are moving on circular epicycles, which, in turn, are orbiting around the sun on perfect circles.
5. A virtual line from the sun to any planet swipes over equal areas in equal amounts of time.
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A line from a planet to the sun sweeps over equal areas in equal intervals of time.
Fas
t Slow
Kepler’s 2nd Law
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History of Astronomy – A one-slide overview
Ptolemy: Copernicus:
Earth in the center (geocentric Universe)
perfect circles
epicycles
Sun in the center (heliocentric Universe)
perfect circles
no epicycles
Galilei:First detailed telescope observations: Moons of Jupiter; rings of Saturn; phases of Venus; sunspots; surface features on the moon -> Support of Copernican model
Kepler:
1. Elliptical orbits
2. Non-uniform velocities
3. Inner planets orbit faster than outer planets
Newton:
1. No force => uniform, straight motion
2. Force = mass*acceleration
3. action = reaction
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The Electromagnetic Spectrum
Need satellites to observe
Wavelength
Frequency
High flying air planes or satellites