today’s apodapod start reading nasa website (oncourse) 2 nd homework due today in-class quiz...
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Today’s APOD
Start Reading NASA website (Oncourse)
2nd Homework due TODAYIN-CLASS QUIZ NEXT FRIDAY!!
The Sun Today
A100 Solar System
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Kepler's Laws were a revolution in regards to understanding planetary motion, but there was no explanation why they worked
The explanation was provided by Isaac Newton when formulated his laws of motion and gravity
Newton recognized that the same physical laws applied both on Earth and in space.
And don’t forget the calculus! Isaac Newton
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Remember the Definitions• Force: the push or pull on an object that
affects its motion• Weight: the force which pulls you toward
the center of the Earth (or any other body)• Inertia: the tendency of an object to keep
moving at the same speed and in the same direction
• Mass: the amount of matter an object has
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Newton's First LawAn object at rest will remain at rest, an
object in uniform motion will stay in motion - UNLESS acted upon by an outside force
Outside Force
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Newton's Second Law
When a force acts on a body, the resulting acceleration is equal to the force divided by the object's mass
Acceleration – a change in speed or direction
Notice how this equation works:The bigger the force, the larger the accelerationThe smaller the mass, the larger the acceleration
m
Fa maF or
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Newton's Third Law
For every action, there is an equal and opposite reaction
Simply put, if body A exerts a force on body B, body B will react with a force that is equal in magnitude but opposite direction
This will be important in astronomy in terms of gravity The Sun pulls on the Earth
and the Earth pulls on the Sun
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Newton and the Apple - Gravity• Newton realized that there
must be some force governing the motion of the planets around the Sun
• Amazingly, Newton was able to connect the motion of the planets to motions here on Earth through gravity
• Gravity is the attractive force two objects place upon one another
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The Gravitational Force
• G is the gravitational constant G = 6.67 x 10-11 N m2/kg2
• m1 and m2 are the masses of the two bodies in question
• r is the distance between the two bodies
221
r
mGmFg
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Determining the Mass of the Sun
How do we determine the mass of the Sun? Put the Sun on a scale and determine its
weight??? Since gravity depends on the masses of both
objects, we can look at how strongly the Sun attracts the Earth
The Sun’s gravitational attraction keeps the Earth going around the Sun, rather than the Earth going straight off into space
By looking at how fast the Earth orbits the Sun at its distance from the Sun, we can get the mass of the Sun
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Measuring Mass with Newton’s Laws - Assumptions to Simplify the
CalculationAssume a small
mass object orbits around a much more massive objectThe Earth around
the SunThe Moon around
the EarthCharon around Pluto
Assume the orbit of the small mass is a circle
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Measuring the Mass of the Sun
The Sun’s gravity is the force that acts on the Earth to keep it moving in a circle
MSun is the mass of the Sun in kilograms MEarth is the mass of the Earth in kilograms r is the radius of the Earth’s orbit in kilometers
The acceleration of the Earth in orbit is given by:a = v2/r
where v is the Earth’s orbital speed
2rmGM
F EarthSung
rv
mamF EarthEarth
2
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Measuring the Mass of the Sun
Set F = mEarthv2/r equal to F = GMSunmEarth/r2
and solve for MSun
MSun = (v2r)/G
The Earth’s orbital speed (v) can be expressed as the circumference of the Earth’s orbit divided by its orbital period:
v = 2r/P
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Measuring the Mass of the Sun Combining these last two equations:
MSun = (42r3)/(GP2)
The radius and period of the Earth’s orbit are both known, G and π are constants, so the Sun’s mass can be calculated
This last equation in known as Kepler’s modified third law and is often used to calculate the mass of a large celestial object from the orbital period and radius of a much smaller mass
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So what is the Mass of the Sun?
MSun = (42r3)/(GP2) rEarth = 1.5 x 1011 meters
PEarth = 3.16 x 107 seconds
G = 6.67 x 10-11 m3 kg-1 s-2
Plugging in the numbers gives the mass of the Sun
MSun = 2 x 1030 kg
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What about the Earth?The same formula gives the mass of the
Earth
Using the orbit of the Moon:rMoon = 3.84 x 105 km
PMoon = 27.322 days = 2.36 x 106 seconds
Mass of Earth is 6 x 1024 kg
MEarth= (42r3)/(GP2)
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How about Pluto?
The same formula gives the mass of Pluto, too
Using the orbit of Pluto’s moon Charon:rCharon = 1.96 x 104 km
PCharon = 6.38 days = 5.5 x 105 seconds
Mass of Pluto is 1.29 x 1022 kilograms
MPluto = (42r3)/(GP2)
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Orbits tell us Mass We can measure the mass of any body that has an
object in orbit around it Planets, stars, asteroids
We just need to know how fast and how far away something is that goes around that object
But we can’t determine the mass of the Moon by watching it go around the Earth
To determine the mass of the Moon, we need a satellite orbiting the Moon
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Surface Gravity
Surface gravity:Determines the weight of a mass at a
celestial object’s surfaceInfluences the shape of celestial objectsInfluences whether or not a celestial
object has an atmosphere
Surface gravity is the acceleration a mass undergoes at the surface of a celestial object (e.g., an asteroid, planet, or star)
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Surface Gravity Calculations Surface gravity is determined from Newton’s Second Law and
the Law of Gravity:ma = GMm/R2
where M and R are the mass and radius of the celestial object, and m is the mass of the object whose acceleration a we wish to know
The surface gravity, denoted by g, is then:g = GM/R2
Notice dependence of g on M and R, but not m
gEarth = 9.8 m/s2
gMoon/gEarth= 0.18
gJupiter/gEarth = 3
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Escape Velocity
To overcome a celestial object’s gravitational force and escape into space, a mass must obtain a critical speed called the escape velocity
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Escape VelocityDetermines if a
spacecraft can move from one planet to another
Influences whether or not a celestial object has an atmosphere
Relates to the nature of black holes
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Escape Velocity Calculation
The escape velocity, Vesc, is determined from Newton’s laws of motion and the Law of Gravity and is given by:
Vesc = (2GM/R)1/2
where M and R are the mass and radius of the celestial object from which the mass wishes to escape
Notice dependence of Vesc on M and R, but not m
Vesc,Earth = 11 km/s, Vesc,Moon = 2.4 km/s
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Revisions to Kepler's 1st Law
• Newton's law of gravity required some slight modifications to Kepler's laws
• Instead of a planet rotating around the center of the Sun, it actually rotates around the center of mass of the two bodies
• Each body makes a small elliptical orbit, but the Sun's orbit is much much smaller than the Earth's because it is so much more massive
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Revisions to Kepler's 3rd Law
Gravity also requires a slight modification to Kepler's 3rd Law
The sum of the masses of the two bodies is now included in the equation
For this equation to work, the masses must be in units of solar mass (usually written as M)
Why did this equation work before?
21
32
MM
aP
Remember - for this equation to work:P must be in years!a must be in A.U.M1 and M2 must be in solar masses
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TO DO LIST:
Start Reading NASA website (Oncourse)
Hand in 2nd Homework TODAYIN-CLASS QUIZ NEXT FRIDAY!!