pertemuan -1 solar system

7/29/2019 Pertemuan -1 Solar System

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Solar System

Suryadi Siregar

Prodi AstronomiITB


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Approximate Typical

Conditions in Galaxy

Region of Interstellar Space

Within our Galaxy

Number Density,

Atoms / cm3

Temperature,*

Kelvins

Inside our Heliosphere,

in the Vicinity of Earth5 10,000

Local Cloud Surrounding

our Heliosphere0.3 7,000

Nearby Void (Local Bubble) < 0.001 1,000,000Typical Star-Forming Cloud >1,000 100

Best Laboratory Vacuum 1000

Classroom Atmosphere 2.7 X 1019 288


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3

Evolution of Solar SystemTheory of Nebular Contraction

Pioneers: Rene de Cartes(1644),

Pierre Simon de Laplace(1796),

Immanuel Kant..

Start with a sphere of gas that is

rotating and contracting, that hasradius of 104Ro, a mean density of

10-12o

contract and rotate until it collapse

into a disk. Central part became the

Sun. Others to be planets Early stages (above). Late stages

(below)


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4

eory o ose ncoun ers etidal Theories)

Pioneers: Georges Louis

de Buffon, Chamberlain

.

Summary: Closestencounter of the stars

attracts the matter of each

stars. Formation of the

planets by thecondensation of material

lost from each star. The

planet revolve the stars


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Theory of Nebular Cluster

The nebula contracts under the

influence of gravitation,

rotational velocity increases

until it collapse into a disk Most massive nebula

concentrate in the center. Mass

density increase, temperature

augmented Sun was born ! Less massive matter ejected to

edge. Forming the planets and

small bodies in solar system


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6

The Solar System Disc Clearance

After the formation of theSun. The residue of matter

continue to rotate, contract

and revolve around the Sun

In early stage thedistribution of matter in the

solar system relatively

homogeny

Step by step theinterplanetary-matter

agglomerates to form the

planets/ protoplanets


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Mass Distribution Within the

Solar System

99.85% Sun

0.135% Planets

0.015% Comets

Kuiper belt objects

Satellites of the planets

Minor Planets (Asteroids)

MeteoroidsInterplanetary Medium


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Residual of primitive cloud


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Jupiter Saturn

Uranus

Neptune

Pluto


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Inferior Planets (r1

AU): high eccentricity,

low density

(Mars, Jupiter, Saturn,

Uranus and Neptune)

Criteria:


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The small and rocky planet Mercury is the closest planet to the Sun; it speeds

around the Sun in a wildly elliptical (non-circular) orbit that takes it as close as 47

million km and as far as 70 million km from the Sun. Mercury completes a trip

around the Sun every 88 days, speeding through space at nearly 50 km per

second, faster than any other planet. Because it is so close to the Sun,temperatures on its surface can reach 467 degrees Celsius. But because the

planet has hardly any atmosphere to keep it warm, nighttime temperatures can

drop to -183 degrees Celsius.

Because Mercury is so close to the Sun, it is hard to see from Earth except during

twilight. Until 1965, scientists thought that the same side of Mercury always facedthe Sun. Then, astronomers discovered that Mercury completes three rotations for

every two orbits around the Sun. The length of one Mercury day (sidereal rotation)

is equal to 58.646 Earth days

Mercury


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Venus

At first glance, if Earth had a twin, it would be Venus. The two planets are similar

in size, mass, composition, and distance from the Sun. But there the similarities

end. Venus has no ocean. Venus is covered by thick, rapidly spinning clouds that

trap surface heat, creating a scorched greenhouse-like world with temperatures

hot enough to melt lead and pressure so intense that standing on Venus would

feel like the pressure felt 900 meters deep in Earth's oceans. These clouds

reflect sunlight in addition to trapping heat. Because Venus reflects so much

sunlight, it is usually the brightest planet in the sky.


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Earth:

Some facts are well known. For instance, Earth is the third planet from the Sun and the

fifth largest in the solar system. Earth's diameter is just a few hundred kilometers larger

than that ofVenus. The four seasons are a result of Earth's axis of rotation being tilted

more than 23 degrees.

The regular daily and monthly rhythms ofEarth's only natural satellite, the Moon, haveguided timekeepers for thousands of years. Its influence on Earth's cycles, notably tides,

has also been charted by many cultures in many ages. More than 70 spacecraft have

been sent to the Moon; 12 astronauts have walked upon its surface and brought back

382 kg (842 pounds) of lunar rock and soil to Earth.

How did the Moon come to be? The leading theory is that a Mars-sized body once hitEarth and the resulting debris (from both Earth and the impacting body) accumulated to

form the Moon. Scientists believe that the Moon was formed approximately 4.5 billion

years ago (the age of the oldest collected lunar rocks). When the Moon formed, its outer

layers melted under very high temperatures, forming the lunar crust, probably from a

global "magma ocean."
http://solarsystem.nasa.gov/planets/profile.cfm?Object=Venushttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Earthhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Earthhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Venus


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Earths Atmosphere

Consists of 5 layers( function oftemperature gradient)

Troposphere

Stratosphere

Mesosphere

ThermosphereExosphere

Composition

-N2 78.084 %

-O2

20.946 %

-A 0.934 %

-CO2 0.035 %

ux1.e

iu.edu


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Mars

Mars is a small rocky body once thought to be very Earth-like. Like the

other "terrestrial" planets - Mercury, Venus, and Earth - its surface has

been changed by volcanism, impacts from other bodies, movements of its

crust, and atmospheric effects such as dust storms. It has polar ice caps

that grow and recede with the change of seasons; areas of layered soils

near the Martian poles suggest that the planet's climate has changed

more than once, perhaps caused by a regular change in the planet's orbit.

Martian tectonics - the formation and change of a planet's crust - differs

from Earth's. Where Earth tectonics involve sliding plates that grind

against each other or spread apart in the seafloors, Martian tectonicsseem to be vertical, with hot lava pushing upwards through the crust to the

surface. Periodically, great dust storms engulf the entire planet. The

effects of these storms are dramatic, including giant dunes, wind streaks,

and wind-carved features
http://solarsystem.nasa.gov/planets/profile.cfm?Object=Mercuryhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Venushttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Earthhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Earthhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Venushttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Mercury


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Mars Atmosphere

Very massive approximately

100x Earths atmosphere

Composition:

-CO2 = 96.5%

-N2 = 3.5%

-SO2 =0.02%

-A = 0.007%

-Ne = 0.001%

Sulfuric acid of cloud and haze

at 30 up to 80 km

physics.uoregon.edu


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Martian soils insitu exploration


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Phobos and Deimos

Asaph Hall,1877


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Main-Belt Asteroids

Sphere of gravitation influence

Scenario the formation of

Phobos and Deimos


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Sphere of gravitation influence

25m

R r

M

R=radius of sphere of influence by a planet

r=heliocentric distance

M=mass of the Sun, m=mass of the planet,


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No Parameter Phobos Deimos

1 r[km] 9377 23436

2 P[day] 0.31891 1.262443 a[km] 26 12

4 b[km] 18 10

5 M[1015kg] 10.8 1.8

6 [kg/m3] 1900 1750

Table . Physical and orbital data of Phobos and Demos


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JupiterThe most massive planet in our solar system, with four planet-sized moons and many

smaller moons, Jupiter forms a kind of miniature solar system. Jupiter resembles astar in composition. In fact, if it had been about eighty times more massive, it would

have become a star rather than a planet.

On January 7, 1610, using his primitive telescope, astronomer Galileo Galilee saw

four small 'stars' near Jupiter. He had discovered Jupiter's four largest moons, now

called Io, Europa, Ganymede, and Callisto. Collectively, these four moons are knowntoday as the Galilean satellites.

Galileo would be astonished at what we have learned about Jupiter and its moons in

the past 30 years. Io is the most volcanically active body in our solar system.

Ganymede is the largest planetary moon and is the only moon in the solar system

known to have its own magnetic field. A liquid ocean may lie beneath the frozen crustof Europa. Icy oceans may also lie deep beneath the crusts of Callisto and

Ganymede. In 2003 alone, astronomers discovered 23 new moons orbiting the giant

planet, giving Jupiter a total moon count of 63 - the most in the solar system. The

numerous small outer moons may be asteroids captured by the giant planet's gravity
http://solarsystem.nasa.gov/planets/profile.cfm?Object=Jup_Europahttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jup_Callistohttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jup_Callistohttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jup_Europa


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SaturnSaturn was the most distant of the five planets known to the ancients. In 1610,

Italian astronomer Galileo Galilei was the first to gaze at Saturn through a

telescope. To his surprise, he saw a pair of objects on either side of the planet.

He sketched them as separate spheres and wrote that Saturn appeared to be

triple-bodied. Continuing his observations over the next few years, Galileo drew

the lateral bodies as arms or handles attached to Saturn. In 1659, Dutch

astronomer Christian Huygens, using a more powerful telescope than Galileo's,

proposed that Saturn was surrounded by a thin, flat ring. In 1675, Italian-born

astronomer Jean-Dominique Cassini discovered a 'division' between what are

now called the A and B rings. It is now known that the gravitational influence of

Saturn's moon Mimas is responsible for the Cassini Division, which is 4,800

kilometers (3,000 miles) wide.

Like Jupiter, Saturn is made mostly of hydrogen and helium. Its volume is 755times greater than that of Earth. Winds in the upper atmosphere reach 500

meters (1,600 feet) per second in the equatorial region. (In contrast, the

strongest hurricane-force winds on Earth top out at about 110 meters, or 360

feet, per second.) These super-fast winds, combined with heat rising from within

the planet's interior, cause the yellow and gold bands visible in the atmosphere.
http://solarsystem.nasa.gov/planets/profile.cfm?Object=Jupiterhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jupiter


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How did the ring of the planet

formed? Roches limit (d)

13

1

2

d 2.5 R

R=radius of planet.

1

= density of planet

2 = density of satellite


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1.Consider an orbiting mass of fluid held together

by gravity, here viewed from above the orbitalplane. Far from the Roche limit the mass is

practically spherical.
http://en.wikipedia.org/wiki/File:Roche_limit_(far_away_sphere).PN


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2. Closer to the Roche limit the

body is deformed by tidal force
http://en.wikipedia.org/wiki/File:Roche_limit_(tidal_sphere).PN


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3.Within the Roche limit the mass's

own gravity can no longer withstandthe tidal forces, and the body

disintegrates.
http://en.wikipedia.org/wiki/File:Roche_limit_(ripped_sphere).PN


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4.Particles closer to the primary

move more quickly than particlesfarther away, as represented by the

red arrows.
http://en.wikipedia.org/wiki/File:Roche_limit_(top_view).PN


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5.The varying orbital speed of thematerial eventually causes it to

form a ring.
http://en.wikipedia.org/wiki/File:Roche_limit_(ring).PN


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Tidal effects on Io


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Table . Roches Limit for planet-satellite system

No Body Satellite Roche Limit(rigid)

[R]

Roche Limit(fluid)

[R]

1 Earth-Moon 1.49 2.86

2 Earth-Comet 2.80 5.39

3 Sun-Earth 0.80 1.53

4 Sun-Jupiter 1.28 2.46

5 Sun-Moon 0.94 1.81

6 Sun-Comet 1.78 3.42


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Table. Radius of Saturns ring (R=60332 km)

No Name Radius [R] Width

[km]

Thick

[km]

Mass

[kg]

Albedo

1 D 1.235 8500

2 C 1.525 17500 1.1 1021 0.1-0,3

3 B 1.949 25500 0.1-1 2.8 1022 0.4-0,6

4 Cassini

Divission

2.025 4700 5.7 1017 0.2-0,4

5 A 2.267 14600 0.1-1 6.2 1021 0.4-0,6

6 F 2.324 30-500 0.6

7 G 2.748 8000 100-

1000

1 1017

8 E 2.983 300000 1000-

30000

7 108


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Uranus

Once considered one of the blander-looking planets, Uranus has been revealed as a

dynamic world with some of the brightest clouds in the outer solar system and 11

rings. The first planet found with the aid of a telescope, Uranus was discovered in

1781 by astronomer William Herschel. The seventh planet from the Sun is so distant

that it takes 84 years to complete one orbit. Uranus, with no solid surface, is one of

the gas giant planets (the others are Jupiter, Saturn, and Neptune).

The atmosphere of Uranus is composed primarily of hydrogen and helium, with a

small amount of methane and traces of water and ammonia. Uranus gets its blue-

green color from methane gas. Sunlight is reflected from Uranus' cloud tops, which

lie beneath a layer of methane gas. As the reflected sunlight passes back throughthis layer, the methane gas absorbs the red portion of the light, allowing the blue

portion to pass through, resulting in the blue-green color that we see. The planet's

atmospheric details are very difficult to see in visible light. The bulk (80 per-cent or

more) of the mass of Uranus is contained in an extended liquid core consisting

primarily of 'icy' materials (water, methane, and ammonia), with higher-density

material at depth.


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Neptune

The eighth planet from the Sun, Neptune was the first planet located throughmathematical predictions rather than through regular observations of the sky.

(Galileo had recorded it as a fixed star during observations with his small

telescope in 1612 and 1613.) When Uranus didn't travel exactly as astronomers

expected it to, a French mathematician, Urbain Joseph Le Verrier, proposed the

position and mass of another as yet unknown planet that could cause the

observed changes to Uranus' orbit. After being ignored by French astronomers, LeVerrier sent his predictions to Johann Gottfried Galle at the Berlin Observatory,

who found Neptune on his first night of searching in 1846. Seventeen days later,

its largest moon, Triton, was also discovered.

Nearly 4.5 billion kilometers (2.8 billion miles) from the Sun, Neptune orbits the

Sun once every 165 years. It is invisible to the naked eye because of its extremedistance from Earth. Interestingly, due to Pluto's unusual elliptical orbit, Neptune is

actually the farthest planet from the Sun for a 20-year period out of every 248

Earth years


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Comet

Throughout history, people have been both awed and alarmed by comets, starswith "long hair" that appeared in the sky unannounced and unpredictably. We now

know that comets are dirty-ice leftovers from the formation of our solar system

around 4.6 billion years ago. They are among the least-changed objects in our

solar system and, as such, may yield important clues about the formation of our

solar system. We can predict the orbits of many of them, but not all.

Around a dozen "new" comets are discovered each year. Short-period comets are

more predictable because they take less than 200 years to orbit the Sun. Most

come from a region of icy bodies beyond the orbit ofNeptune. These icy bodies are

variously called Kuiper Belt Objects, Edgeworth-Kuiper Belt Objects, or trans-

Neptunian objects. Less predictable are long-period comets, many of which arrive

from a distant region called the Oort cloud about 100,000 astronomical units (thatis, 100,000 times the mean distance between Earth and the Sun) from the Sun.

These comets can take as long as 30 million years to complete one trip around the

Sun. (It takes Earth only 1 year to orbit the Sun.) As many as a trillion comets may

reside in the Oort cloud, orbiting the Sun near the edge of the Sun's gravitational

influence.
http://solarsystem.nasa.gov/planets/profile.cfm?Object=Neptunehttp://solarsystem.nasa.gov/planets/profile.cfm?Object=KBOshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=KBOshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Neptune


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Kuiper Belt Object

The Kuiper Belt is often called our Solar System's 'finalfrontier.' This disk-shaped region of icy debris is about 4.5 to

7.5 billion km (2.8 billion to 4.6 billion miles), 30 to 50

Astronomical Units (AU). from our Sun. Its existence

confirmed only a decade ago, the Kuiper Belt and itscollection of icy objects - KBOs - are an emerging area of

research in planetary science.

No spacecraft has ever traveled to the Kuiper Belt, but

NASA's New Horizons mission, planned to arrive at Pluto in

2015, might be able to penetrate farther into the Kuiper Belt

to study one of these mysterious objects.


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Dwarfs Planet

What Defines a Planet?

What constitutes a planet? The International Astronomical Union (IAU) developed somedefinitions in 2001, modified them again in 2003, and as of August 24, 2006, the IAU has

come up with another definition. The IAU said in a statement that the definition for a planet

is now officially known as "a celestial body that (a) is in orbit around the Sun, (b) has

sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a

hydrostatic equilibrium (nearly round) shape and (c) has cleared the neighborhood around

its orbit."

A "dwarf planet" is a celestial body that (a) is in orbit around the Sun, (b) has sufficient mass

for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium

(nearly round) shape, (c) has not cleared the neighborhood around its orbit, and (d) is not a

satellite.

All other objects except satellites orbiting the Sun shall be referred to collectively as "SmallSolar-System Bodies". According to the IAU, more dwarf planets are expected to be

announced in the coming months and years. Currently, a dozen candidate dwarf planets are

listed on IAU's dwarf planet watch list, which keeps changing as new objects are found and

the physics of the existing candidates becomes better-known.


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Oort Cloud

The Oort Cloud is an immense spherical cloud surrounding our Solar System.Extending about 30 trillion kilometers (18 trillion miles) from the Sun, it was first

proposed in 1950 by Dutch astronomer Jan Oort. The vast distance of the Oort

cloud is considered to be the outer edge of the Solar System - where the Sun's

orb of physical and gravitational influence ends.

The Oort Cloud contains billions of icy bodies in solar orbit. Occasionally,

passing stars disturb the orbit of one of these bodies, causing it to comestreaking into the inner solar system as a long-period comet. These comets have

very large orbits and are observed in the inner solar system only once. In

contrast, short-period comets take less than 200 years to orbit the Sun and they

travel along the plane in which most of the planets orbit. They come from a

region beyond Neptune called the Kuiper Belt, named for astronomer Gerard

Kuiper, who proposed its existence in 1951.

In 1991 radio astronomers detected the first extra solar planets orbiting a dying

pulsar star. Although the deadly radiation from the pulsar is not condusive to life,

it was the first example of a star other than our Sun producing planets.


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PlutoStory of Pluto:

On August 24, 2006, the International Astronomical Union (IAU) formally downgraded Plutofrom an official planet to a dwarf planet. According to the new rules a planet meets three

criteria: it must orbit the Sun, it must be big enough for gravity to squash it into a round ball,and it must have cleared other things out of the way in its orbital neighborhood. The lattermeasure knocks out Pluto and 2003UB313 (Eris), which orbit among the icy wrecks of the

Kuiper Belt, and Ceres, which is in the asteroid belt.

(1) A "planet" is a celestial body that (a) is in orbit around the Sun, (b) has sufficient mass for itsself-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly

round) shape, and (c) has cleared the neighborhood around its orbit.

(2) A "dwarf planet" is a celestial body that (a) is in orbit around the Sun, (b) has sufficient massfor its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium(nearly round) shape, (c) has not cleared the neighborhood around its orbit, and (d) is not a

satellite.

(3) All other objects except satellites orbiting the Sun shall be referred to collectively as "SmallSolar-System Bodies".


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Main Belt and Trojan Asteroid


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Formation of Asteroids

1. Forming by the rest of

primordial cloud that

cannot became a

planet. Criteria;

spherical form, low

eccentricity, orbit

relatively stable.

Founded between

Mars and Jupiter

2. Forming by collision

between asteroid inmain belt. Criteria;

irregular form, orbit not

stable, high

eccentricity, crosser

orbit of the planet

Lagrangian Points=Equilibrium position


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Since the invention of the telescope, three more planets have been

discovered in our solar system: Uranus (1781), Neptune (1846), and Pluto(1930). [Now Pluto's status as a "dwarf planet".] In addition, there are

thousands of small bodies such as asteroids and comets. Most of the

asteroids orbit in a region between the orbits ofMars and Jupiter, while the

home of comets lies far beyond the orbit of Pluto, in the Oort Cloud.

The four planets closest to the Sun - Mercury, Venus, Earth, and Mars - arecalled the terrestrial planets because they have solid rocky surfaces. The

four large planets beyond the orbit of Mars - Jupiter, Saturn, Uranus, and

Neptune - are called gas giants. Tiny, distant, Pluto has a solid but icier

surface than the terrestrial planets.

f
http://solarsystem.nasa.gov/planets/profile.cfm?Object=Uranushttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Neptunehttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Plutohttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Asteroidshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Cometshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Sunhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Mercuryhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Venushttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Earthhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jupiterhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Saturnhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Saturnhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jupiterhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Earthhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Venushttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Mercuryhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Sunhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Cometshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Asteroidshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Plutohttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Neptunehttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Uranus


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Revolution and Rotation of

the Earth


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Global Warming


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Milankovitch CycleMilankovitch cycles are the collective effect of changes in the Earth's

movements upon its climate, named after Serbian civil engineer and

mathematician Milutin Milankovi. The eccentricity, axial tilt, and precession of

the Earth's orbit vary in several patterns, resulting in 100,000-year ice age cycles

of the Quaternary glaciation over the last few million years. The Earth's axis

completes one full cycle of precession approximately every 26,000 years. At the

same time, the elliptical orbit rotates, more slowly, leading to a 21,000-year cycle

between the seasons and the orbit. In addition, the angle between Earth'srotational axis and the normal to the plane of its orbit moves from 22.1 degrees

to 24.5 degrees and back again on a 41,000-year cycle. Currently, this angle is

23.44 degrees and is decreasing.

The Milankovitch theory of climate change is not perfectly worked out; in

particular, the largest observed response is at the 100,000-year timescale, but

the forcing is apparently small at this scale, in regard to the ice ages. Variousfeedbacks (from carbon dioxide, or from ice sheet dynamics) are invoked to

explain this discrepancy.

Milankovitch-like theories were advanced by Joseph Adhemar, James Croll and

others, but verification was difficult due to the absence of reliably dated evidence

and doubts as to exactly which periods were important.


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Oort cloud, Kohoutek

orbit ,Gaspra asteroid

and Neat comet

Short-period comets: P< 200

yrs. Elliptical orbit

Long-period comets: P>200

yrs. Orbit: elliptical,parabolic or

hyperbolic


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S d M


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Second Moon

Category Near-Earth asteroid,

Venus-crosser asteroid,

Mars-crosser asteroid

Orbital Epoch May 14, 2008 Aphelion=1.51AU.Perihelion=0.484

AU.Semi-major axis=0.998 AU.Eccentricity=0.515.Orbital

period=363.99 d Average orbital speed=27.73 km/s Meananomaly=134.76. Inclination=19.81.Longitude of

ascending node= 126.28Argument of perihelion= 43.74

Physical Diameter~5 km. Mass=1.31014 kg. Mean density= 2 ?

g/cm. Equatorial surface gravity = 0.0014 m/s . Escapevelocity= 0.0026 km/s. Rotation period= 27.44 h Albedo=

0.15 ?. Temperature~275 K. Spectral type?. Absolute

magnitude (H)=15.1
http://en.wikipedia.org/wiki/File:Orbits_of_Cruithne_and_Earth.gifhttp://en.wikipedia.org/wiki/File:Orbits_of_Cruithne_and_Earth.gifhttp://en.wikipedia.org/wiki/File:Orbits_of_Cruithne_and_Earth.gifhttp://en.wikipedia.org/wiki/File:Orbits_of_Cruithne_and_Earth.gifhttp://en.wikipedia.org/wiki/File:Horseshoe_orbit_of_Cruithne_from_the_perspective_of_Earth.gifhttp://en.wikipedia.org/wiki/File:Orbits_of_Cruithne_and_Earth.gif


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1898 -> First Amor

1976 -> First Aten

Near Earth Asteroids (NEAs):Amors, Apollos, and Atens

Source: Main belt and Mars-crossers

Near Earth Objects (NEOs)


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Near-Earth Objects (NEOs)

T i l


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1-Opposition

2-Quadrature Western

3-Quadrature Eastern

4-Superior Conjunction

5-Superior Conjunction

6-Maximum Elongation(Western)

7-Maximum Elongation

(Eastern)

8-Inferior ConjunctionEarths Orbit

5

4

3

2

1

Inferior Planet

Superior Planet

Terminology

8Earth

7

6

5


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In the Universe of Kepler & Newton

Planets move on ellipses around Sun

space is flat:

Gravity is interaction between masses

O bit l l E li ti l


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Orbital plane-Ecliptic plane

Ecliptic plane

Orbital plane

North

iPlanet(r,)

Sun


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2

2

221

m

Ehe

)(1

)1( 2

eCos

ear

GM

)211(22

arGMV

h = 2 x area/unit time =

Keplers constant

The Orbit-1


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58

)(1

)1( 2

eCos

ea

r

In Solar System

= r = a(1-e) minimum distance, perihelion

- = 1800 r = a(1+e) maximum distance, aphelion

Kepler-1

Kepler-2 rvrvSinvrh

The Orbit-2

Th O bit 3


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59

The Orbit-3

2

22

21 0

Eh

m

Eccentricity

(a)

(b)

(c)

(d)

m1 m1

m1m1

m2

m2 m2

m2

E=Kinetic Energy+Potential Energy

E = 0 , then e = 1 trajectory is parabolic

E < 0 , then e < 1 trajectory is ellips

E > 0 , then e > 1 trajectory ishiperbolic

2

2mEr

2

2

221

m

Ehe

Circle orbit

2

2

mE

a

Elliptic Orbit

2

2

mE

a

Hyperbolic Orbit

1 2( )G m m 2 1 21 1

2 ( )2

V G m mr a

Orbital characteristics of the planets


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Orbital characteristics of the planets

No Planet a[AU] P[y] e[.] P2/a3 Psin [d]

1 Mercury 0.387 0.241 0.206 1.002 115.9

2 Venus 0.723 0.615 0.007 1.001 583.95

3 Earth 1.000 1.000 0.017 1.000 -

4 Mars 1.524 1.881 0.093 1.000 780.012

5 Jupiter 5.203 11.86 0.048 0.999 393.85

6 Saturn 9.539 29.46 0.056 1.000 373.05

7 Uranus 19.19 84.07 0.046 1.000 369.65

8 Neptun

e

30.06 164.82 0.010 1.000 367.45


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Instability of Mercurys perihelion

I th U i f Ei t i


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In the Universe of Einstein Matter determines how space curves. Curved space determines how matter moves. Space & time cannot be separated: space-time Gravity is interaction between space-time and mass.

How to test Einstein?


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Einsteins theory of gravity is called General relativity Gravity is weak! Compare to electrical force:

Need massive bodies!

Try astronomical bodies like planets & Sun!

Proton Electron

3910 1,000,000,000,000,000,000,000,000,000,000,000,000,000elc

grav

F

F



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How to test Einstein?The first test: The precession of Mercurys orbit

General relativity theory can correctly predictprecession rate!

0.012 deg/century

One full rotation takes 3 million years!

P i d N t ti d t th


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Precession and Nutation: due to the

gravitational attractions of Sun and Moon

on the rotating,non-spherical Earth


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Sidereal Priode and Synodic Priode

Sidereal Priode : Time interval between

successive similar configurations of the object,

the Earth and the Star

Synodic Priode : Time interval betweensuccessive similar configurations of the object,

the Sun and the Earth. Example: opposition to

opposition, new moon to new moon

1 1 1


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Inferior Planet;

sin si

1 1 1

dP P P Superior Planet

Moonsin si

1 1 1

dP P P

Earths Psid = 365,25 days. Venus Psid= 224,7 days

Mars Psid =687 days. Moons Psid = 27,32 days

Venus Psin = 583,93 days

Moon Psin =29,53 days

Mars Psin=779,88 days= 780 days

sin si

1 1 1

dP P P


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sin si

1 1 1

dP P P

Moons Psin =29,53 days

Earths Psid = 365,25 days

Moons Psid = 27,32 days

Moons phase

1

12

q Cos

= phase angle= 180 q =0 new Moon

= 0 q = 1 Full Moon

= 90 q=0,5 Quarter moon

=0oMoons Phase


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O CBA

C

=180o

New Moon , q=0

SunFull Moon q=1

Moon

Earth

D

E

q = Ratio of brightness surface

OBCDE:ABCDE=AC':AB

1

12

q Cos

Moon s Phase


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Zodiac

Constellations for Southern Hemisphere


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Constellations for Southern Hemisphere

Summer Winter

Night and day


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Night and day

0Cost Tg Tg

t0half arc of day

-Suns declination

-observers latitude

Cases;

Observer at equator=00 t0= 900 arc

of day = 1800=12 jam

Sun at equator=00 t0= 900 arc of

day = 1800=12 jam

Observer at pole =900 and 00 t0 -

undefinition, arc day so no

Sunrise/Sunset

Planet and Satellite


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PlanetNamed by

the IAU

Provisionally

NamedTotal Moons

Mercury 0 0 0

Venus 0 0 0

Earth 1 0 1

Mars 2 0 2

Jupiter 38 25 63

Saturn 35 21 56

Uranus 27 0 27Neptune 9 4 13

Total Moons 112 50 162

Body TypeNamed by

the IAU

Provisionally

Named

Total objects

Known Dwarf Planets 2 1 3

Dwarf Planet Watch List 6 6 12

Grand Total 120 57 177

Data Mercur Venu Earth Mars Jupiter Saturn Uranu Neptun


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y s s e

r[au] 0,387 0,723 1 1,524 5,203 9,539 19,18 30,06

Po[d] 0,29 0,61 1 1,88 11,86 29,46 84,01 164,8

Pr[d] 59 243 1 1,03 0,41 0,44 0,68 0,83

V 1,61 1,17 1 0,81 0,44 0,32 0,23 0,18


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Earths magnetic field

mscf.nasa.gov

G h Eff t i V


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76

Greenhouse Effect in Venus

physics.uoregon.edu


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From Meteoroid To

Meteorite


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Story of Meteorite

Meteoroids


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Meteoroids

Scientists estimate that 1,000 tons to more than 10,000tons of meteoritic material falls on the Earth each day.

However, most of this material is very tiny - in the form of

micrometeoroids or dust-like grains a few micrometers in

size. (These particles are so tiny that the air resistance is

enough to slow them sufficiently that they do not burn up,

but rather fall gently to Earth.)

Where do they come from? They probably come from

within our own solar system, rather than interstellar

space. Their composition provides clues to their origins.

They may share a common origin with the asteroids.

Some meteoritic material is similar to the Earth and Moon

and some is quite different. Some evidence indicates an

origin from comets.

Solar WindFlows out from the corona


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Earths

magnetosphere

Continuously, in all directions Impacts Earths magnetic field

Image credit: K. Endo, Nikkei Science Inc.


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SEAMEO CENTRE FOR QITEP IN SCIENCE

The Heliosphere


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The Heliosphere

Beyond Our Solar System


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Beyond Our Solar SystemIn 1991, the nine worlds of our own solar system were the only known planets.

Astronomers did not believe that ourSun's environment was the only planet

producer in the universe. But they had no evidence of planets outside our solarsystem.

How quickly things change.

In 1991 radio astronomers detected the first extra solar planets orbiting a dying

pulsar star. Although the deadly radiation from the pulsar is not condusive to life,it was the first example of a star other than our Sun producing planets.

Since then more than 100 planets have been found orbiting other stars. Some of

them are orbiting extremely close to their parent star like the 51 Pegasi

planetary system, while others are found to be at distances comparable to

where Mars and Jupiterorbit in our solar system.Since then more than 100 planets have been found orbiting other stars. Some of

them are orbiting extremely close to their parent star like the 51 Pegasi

planetary system, while others are found to be at distances comparable to

where Mars and Jupiterorbit in our solar system.

83
http://solarsystem.nasa.gov/planets/profile.cfm?Object=Sunhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jupiterhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jupiterhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jupiterhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jupiterhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Sun


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85 THANK YOUTSE-TSE

MERCY

DANKEGRACY

ARIGATO KOZAIMAS

pertemuan -1 solar system

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