Tycho Brahe (1546-1601)
Foremost astronomer after the death of Copernicus. King Frederick II of Denmark set him up at Uraniborg, an observatory on the island of Hveen.
With new instruments (quadrant), Brahe could measure positions of stars and planets to 4 minutes of arc (1/8th the diameter of the full moon).
With new instruments (quadrant, similar to present-day sextant), Brahe could measure positions of stars and planets to better than 4 minutes of arc (1/8th the diameter of the full moon). Made the most accurate observations of planet positions ever recorded.
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Using the Quadrant (similar to a Sextant) to measure a star’s altitude. An observer
sights a star along the Quadrant while a plumb line
measures the angle.
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Tycho Brahe (1546-1601)
Also Credited with observing the supernova of 1572, demonstrating that the stars do change. He coined the term “Nova” for “new star” in a book. Term still used today.
Brahe failed to find evidence for the Earth’s motion and presumed the Copernican model was false. Brahe endorsed the Geocentric cosmology.
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Johannes Kepler (1571-1630)
Brahe moved to Prague in 1599. Kepler joined him to develop cosmological model consistent with Brahe’s observations.
Kepler initially obtained excellent agreement with Brahe’s data with the planets moving in spheres and equants, similar to Ptolemy’s model, except for 2 data points which were off by 8 minutes of arc (twice the accuracy of Brahe’s measurements).
Kepler kept struggling and finally rejected Ptolemaic model and eventually realized that that Brahe’s data were only consistent with a model where planets (1) orbit the Sun and (2) their orbits are ellipses.
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Observed Planetand uncertainty on the measurement
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Observed Planetand uncertainty on the measurement
Position Predicted by Model
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Johannes Kepler (1571-1630)
Kepler’s Laws: published in 1609 in Astronomica Nova (The New Astronomy).
1st Law: A planet orbits the Sun in an ellipse, with the Sun at one focus of the ellipse.
2nd Law: A line connecting a planet to the Sun sweeps out equal areas in equal time intervals.
3rd Law: The square of the orbital period, P, of a planet is equal to the cube of the average distance, a, of the planet from the Sun.
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Ellipses
Sun
PerihelionAphelion
defines an ellipse
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Sir Isaac Newton (1643-1727)
Developed Universal theory of Gravity, and set his three Laws of Motion, which are framework for classical mechanics, including basis for modern engineering.
-1st Law: An object at rest, remains at rest unless acted on by an outside force. An object with uniform motion, remains in motion unless acted on by an oustide force.
- 2nd Law: An applied force, F, on an object equals the rate of change of its momentum, p, with time.
- 3rd Law: For every action there is an equal and opposite reaction.
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Newton’s Theory of GravityStart with Kepler’s 3rd law:
For circular orbit:
Insert this into Kepler’s 3rd law:
Multiply both sides by factors:
Yields: Force !
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Newton’s Theory of Gravity
By Newton’s 3rd law, this is the force on mass M from mass m, so the force on mass m should be:
Equating these two formula gives:
where and
Defining we get the “usual” formula:
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Define Center of Mass Frame
by Newton’s 3rd Law
for 2 objects
for i=1..N objects
Differentiate with time,
Derive Kepler’s Laws from Newton’s Laws
Differentiate with time, again:
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Choose Frame with R=0
Define “Reduced Mass” of the System : μ= m1 m2 / (m1+m2)
Derive Kepler’s Laws from Newton’s Laws
=0
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r = r’2 - r’1
Now write out total Energy of the System
Insert:
And :
Derive Kepler’s Laws from Newton’s Laws
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Total Energy Becomes:
And:
Grouping Terms :
Total Energy of the System is the sum of the Kinetic Energy of the reduced mass and the potential energy of the total mass/reduced mass system.
Derive Kepler’s Laws from Newton’s Laws
Which Gives:
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Introduce Angular Momentum:
Look at rate-of-change of L as a function of t:
= 0 , Conservation of Angular Momentum
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Similarly for the Angular Momentum:
Insert:
Leads to:
The Two-Body problem may be treated as a One-body problem with μ moving about a fixed
mass M at a distance r.
Derive Kepler’s Laws from Newton’s Laws
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Johannes Kepler (1571-1630)
Kepler’s Laws: published in 1609 in Astronomica Nova (The New Astronomy).
1st Law: A planet orbits the Sun in an ellipse, with the Sun at one focus of the ellipse.
2nd Law: A line connecting a planet to the Sun sweeps out equal areas in equal time intervals.
3rd Law: The square of the orbital period, P, of a planet is equal to the cube of the average distance, a, of the planet from the Sun.
P2 = Constant x a3
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Ellipses
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Ellipses
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Eccentricity
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Eccentricity
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Eccentricity=1Parabolic orbit(goes through perihelion only once)
Eccentricity
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Kepler’s First Law
Each planet moves on an elliptical orbit with the Center of Mass (the Sun) at one focus:
Perihelion distance = (1-eccentricity) x (semimajor axis)
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Kepler’s First Law
Each planet moves on an elliptical orbit with the Center of Mass (the Sun) at one focus:
“Perilously close”
Perihelion distance = (1-eccentricity) x (semimajor axis)
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Planets Follow Eliptical Orbits
The Inner Solar System The Outer Solar System
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Not just planets! Comets have elliptical orbits too.
Kepler’s First Law
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Not just planets! Comets have elliptical orbits too.
Halley’s Comet (76 yr orbit)
Kepler’s First Law
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Not just planets! Comets have elliptical orbits too.
Halley’s Comet (76 yr orbit)
Halley’s Comet in 2024
Kepler’s First Law
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Kepler’s Second LawEqual Areas = Equal TimesConservation of Angular Momentum
Near perihelion, in any particular amount of time (such as 30 days) a planet sweeps out an area that
is short by wide.
Near aphelion, in the same amount of time (such as 30 days) a planet sweeps out an area that is long by narrow.
The areas swept out during any 30-day period are all equal
perihelion
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Kepler’s Second LawEqual Areas = Equal TimesConservation of Angular Momentum
The areas swept out during any 30-day period are all equal
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Velocity Inversely Proportional to Orbital Radius
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Kepler’s Third LawSquare of orbital periods (P) is proportional tocube of semi-major axis (a): P
2! a
3
Jupiter
Saturn
Average distance cubed (AU3) from Sun.
Orb
ital P
erio
d sq
uare
d (y
ears
2 )
Semimajor axis
MercuryEarth
Mars
Venus
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Kepler’s Third Law
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Orbital Period vs Orbital Radius
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The Two-Body problem may be treated as a One-body problem with μ moving about a fixed
mass M at a distance r.
Derive Kepler’s Laws from Newton’s Laws
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A x (B x C) = (A·C) ·B - (A·B)·C
Derive Kepler’s Laws from Newton’s Laws
Take cross product:
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D is a constant
v x L and r lie in the same plane, so must D
D is directed toward Perihelion,
D determines e (eccentricity) of ellipse.
Maximum reached with r and D point in same direction.
^
^
Derive Kepler’s Laws from Newton’s Laws
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A · (B x C) = (A x B)·C
Kepler’s 1st Law !
Derive Kepler’s Laws from Newton’s Laws
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^
= Kepler’s 2nd Law !
Integrate from Focus to r: dA = ½ r2 dθ
dAdt
= ½ r2 dθdt
Let : v = vr + vθdrdt
r + r dθdt θ
^=dAdt
= ½ r vθ
r and vθ are perpendicular, therefore : r vθ = |r x v| = | L / μ | = L / μ
dAdt
L2μ = Constant
Derive Kepler’s Laws from Newton’s Laws
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Integrate 2nd Law with time: A = ½ L/μ ∫dt
A = ½ (L/μ) P, where P = period
A = π ab
P2 = 4π2 a2 b2 μ2
L2
r = L2 / μ2
GM (1 + e cosθ)1st Law: L = μ [ GMa (1-e2) ]½
P2 = 4π2 a3
G (m1 + m2)Kepler’s 3rd Law
Derive Kepler’s Laws from Newton’s Laws
a
b
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Calculate Orbital Speed at Perihelion and Aphelion
SunPerihelionAphelion
Use Kepler’s 1st Law
Total Energy:
At Perihelion
At Aphelion
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Total Energy in a Bound Orbit
Etot =-GMμ
2a =
-Gm1m2
2a = <U> / 2
That is the total energy is 1/2 of the average potential energy.
This is the Virial Theorem.
More in depth derivation by Rudolf Clausius (reproduced in book). It has many applications
in astrophysics, including providing evidence for Dark
Matter in Clusters of Galaxies !
Rudolf Julius Emanuel Clausius (January 2, 1822 – August 24, 1888), was a German physicist. He is one of the central founders of the science of thermodynamics.
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High Tide in Bay of Bundy
Low Tide
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What Causes Ocean Tides ?
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Saturn as seen by Spacecraft Cassini, October 2004
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Fc,x = -G Mm / r2 Fc,y = 0
Fp,x = (G Mm/s2 )cosϕ Fp,y = -(G Mm/s2 )sinϕ
ΔF = Fp - Fc = G Mm cosϕ
s2 r21
i - G Mms2 sinϕ j^ ^( ( ))-
s2 = (r - Rcosθ)2 + (Rsinθ)2 = r2 1 - 2Rcosθr
( ) R << r
Tidal Forces
M= mass of Moon; m= test mass
Force of Moon on m at center of
Earth
Force of Moon on m on surface of
Earth
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ΔF ≈ G Mm/r2 [ cosϕ 1 +
Tidal Forces
ΔF = Fp - Fc = G Mm cosϕ
s2 r21
i - G Mms2 sinϕ j^ ^( ( ))-
s2 = (r - Rcosθ)2 + (Rsinθ)2 = r2 1 - 2Rcosθr
(
) R << r
2Rcosθr ) -1 ] i
(
^
- G Mm/r2 [ 1 + 2Rcosθr ] sinϕ j
For the Earth-Moon, cosϕ ≈1, r sin ϕ = Rsinθ, sin ϕ = (R/r) sinθ
ΔF ≈ G MmR/r3 [ 2cosθ i - sinθ j ] ^ ^
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Tidal Forces
ΔF ≈ G MmR/r3 [ 2cosθ i - sinθ j ] ^ ^
Force of the Moon on the Earth
Differential (relative) force on the Earth,
relative to the center
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When will the tidal force equal the force of gravity ? Consider the Earth-Moon system:
Mm, Rm = mass of moon, radius of moon
ME, RE = mass of Earth, radius of Earth
Tidal Forces
ΔF ≈ G MmR/r3 [ 2cosθ i - sinθ j ] ^ ^
G Mmm/Rm2 = ( 2GMEm/r3 ) Rm
Assume constant density: Mm = (4/3)πRm3 ρm
r3 = (2ME/Mm ) Rm3 = (2RE3 ρE) / (Rm3 ρm) Rm3
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r3 = (2ME/Mm ) Rm3 = (2RE3 ρE) / (Rm3 ρm) Rm3
Tidal ForcesG Mmm/Rm2 = ( 2GMEm/r3 ) Rm
Assume constant density: Mm = (4/3)πRm3 ρm
r = ( )⅓2ρE
ρmRE
Roche, using a more sophisticated assumption for the density of the Moon calculated fR = 2.456
r = fR ( )⅓ρE
ρmRE, fR = 2 ⅓ =1.2599
or
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Comet Shoemaker-Levy 9 after passing through Jupiter’s Roche Limit
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Saturn as seen by Spacecraft Cassini, October 2004
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Other MoonsJanus
Epimetheus
DioneRhea
Distance from Saturn Center in RS
1 2 3 4 5 6 7 8
RingsRings
Saturn
Roche Limit
Mimas Enceladas Tethys
Rings
Planetary Moons form when a moon crosses the Roche Limit
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How do you know the Earth Rotates ?
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How do you know the Earth Rotates ?
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How do you know the Earth Rotates ?
In 1851, Léon Foucault proved the Earth’s rotation directly.
A pendulum swinging on the Earth feels the rotation due to the Coriolis Force.
FC = -2 m Ω x v
Versions of the Foucault Pendulum now swings in the Panthéon of Paris
and the Houston Museum of Natural Science
http://www.youtube.com/watch?v=CpxDAdtJX2s
http://www.youtube.com/watch?v=49JwbrXcPjc
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How do you know the Earth Rotates ?
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How do you know the Earth Rotates ?
Coriolis Force affects rotation of weather patterns (cyclones rotate counter clockwise in southern hemisphere; hurricanes rotate clockwise in northern hemisphere).
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How do you know the Earth Rotates ?
Hurricane GustavAug 31, 2008
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How do you know the Earth Rotates ?
Coriolis Force affects rotation of weather patterns (cyclones rotate clockwise in southern hemisphere; hurricanes rotate counter-clockwise in northern hemisphere).
Hurricane GustavAug 31, 2008
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