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Resonance In the SolarSystem
Steve Bache
UNC WilmingtonDept. of Physics and Physical Oceanography
Advisor : Dr. Russ Herman
Spring 2012
Goal
• numerically investigate the dynamics of the asteroid belt
• relate old ideas to new methods
• reproduce known results
History
The role of science:
• make sense of the world
• perceive order out of apparent randomness
• the sky and heavenly bodies
History
The role of science:
• make sense of the world
• perceive order out of apparent randomness
• the sky and heavenly bodies
Anaximander (611-547 BC)• Greek philosopher, scientist• stars, moon, sun 1:2:3
Figure: Anaximander’s Model
Pythagoras (570-495 BC)
• Mathematician, philosopher, started a religion
• all heavenly bodies at whole number ratios
• ”Harmony of the spheres”
Figure: Pythagorean Model
Tycho Brahe (1546-1601)
• Danishastronomer,alchemist
• accurateastronomicalobservations, notelescope
• importance ofdata collection
Johannes Kepler (1571-1631)
• Brahe’s assistant
• Used detailed data provided by Brahe
• Observations led to Laws of Planetary Motion
• orbits are ellipses• equal area in equal time• T 2 ∝ a3
Johannes Kepler (1571-1631)
• Brahe’s assistant
• Used detailed data provided by Brahe
• Observations led to Laws of Planetary Motion• orbits are ellipses• equal area in equal time• T 2 ∝ a3
Kepler’s Model
• Astrologer, Harmonices Mundi• Used empirical data to formulate laws
Figure: Kepler’s Model
Isaac Newton (1642-1727)
• religious, yet desired a physical mechanism to explain Kepler’slaws
• contributions to mathematics and science• Principia• almost entirety of an undergraduate physics degree• Law of Universal Gravitation
~F12 = −G m1m2
|r12|2r12.
Resonance
• Transition from ratios/ integer spacing to more physicaldescription, resonance plays a key role in celestial mechanics
• Commensurability
The property of two orbiting objects, such as planets, satellites, orasteroids, whose orbital periods are in a rational proportion.
• ResonanceOrbital resonances occur when the mean motions of two or morebodies are related by close to an integer ratio of their orbitalperiods
Resonance
• Transition from ratios/ integer spacing to more physicaldescription, resonance plays a key role in celestial mechanics
• Commensurability
The property of two orbiting objects, such as planets, satellites, orasteroids, whose orbital periods are in a rational proportion.
• ResonanceOrbital resonances occur when the mean motions of two or morebodies are related by close to an integer ratio of their orbitalperiods
Resonance
• Transition from ratios/ integer spacing to more physicaldescription, resonance plays a key role in celestial mechanics
• Commensurability
The property of two orbiting objects, such as planets, satellites, orasteroids, whose orbital periods are in a rational proportion.
• ResonanceOrbital resonances occur when the mean motions of two or morebodies are related by close to an integer ratio of their orbitalperiods
Kirkwood Gaps
• Commensurability in the orbital periods cause an ejection byJupiter
• explanation provided by Kirkwood, using 100 asteroids
• now thought to exhibit chaotic change in eccentricity
My Goal
• To create a simulation of the interactions of Jupiter, the Sun,and ’test’ asteroids
• Integrate Newton’s equations of motion in MATLAB over alarge time span (≈ 1MY )
Requirements
1 an idea for what causes orbital resonance
2 an appropriate integrating scheme
3 initial conditions for all bodies being considered
• Start with the Kepler problem
Requirements
1 an idea for what causes orbital resonance
2 an appropriate integrating scheme
3 initial conditions for all bodies being considered
• Start with the Kepler problem
Kepler Problem
• The problem of two bodies interacting only by a central forceis known as the Kepler Problem
• Also known as the 2-body problem
Kepler Problem
m1r1 = Gm1m2
r212= G
m1m2(r1 − r2)
r312
m2r2 = Gm1m2
r212= G
m1m2(r2 − r1)
r312
Center of Mass is stationary/ moves at constant velocity
Classic treatment
Considering motion of m2 with respect to m1 gives:
r× r = 0,
which, integrating once, gives
r × r = h
This implies that
the motion in the two-body problem lies in a plane.
Treat this relative motion in polar coordinates (r,θ).
Polar form
Using,
r = r r
r = r r + r θθ
r = (r − r θ)r +
[1
r
d
dt(r2θ)
]θ,
one finds the solution:
r(θ) =p
1 + e cos(θ),
where p = h2
µ .
Kepler’s Laws
1 The motion of m2 is an ellipse with m1 at one focus
2dAdt = h
2 = constant
Figure: Kepler’s 2nd Law
Kepler’s third law
• From Kepler’s second law, we have dAdt = h
2 .
• area of ellipse = A = πab
• τ = AdAdt
3 τ2 = 4π2a3
µ , or τ2 ∝ a3.
N-Body Problem
• no analyticalsolutions forN > 2
• computationalmethods →Euler’s method,Runge-Kutta
• need a bettermethod
N-Body Problem
• no analyticalsolutions forN > 2
• computationalmethods →Euler’s method,Runge-Kutta
• need a bettermethod
System
• N bodies - Sun, Jupiter, asteroids
• centralized force
• kinetic and potential energies independent
• Hamiltonian system
N-Body Hamiltonian
• Hamiltonian is separable, i.e. H = H(q, p, t) = T (p) + U(q)
T =1
2
n∑i=1
p2imi
U = −N∑i=2
i−1∑j=1
Gmimj
|q1 − qj |
N-Body Hamiltonian
• from Hamilton equations:
qi = ∇piH =pimi
pi = ∇qiH = −Gmi
n∑j 6=i
mj(qi − qj)
|qi − qj |3
Numerical Scheme
• best approach → symplectic integrator
• designed for solutions to Hamiltonian systems
• preserves volume in phase space
Derivation
To derive the simplectic integrator to be used, compose Eulermethod map
qi+1 = qi + dt∇piH
pi+1 = pi − dt∇qi+1H
with its adjointpi+1 = pi − dt∇qiH
qi+1 = qi + dt∇pi+1H
by introducing a ”half time step” i + 12 of size dt
2 .
Derivation
New integrating scheme is now
qi+ 12
= qi +dt
2∇piH
pi+1 = pi − dt∇qi+1
2
H
qi+1 = qi+ 12
+dt
2∇pi+1H.
Leapfrog Algorithm
• additional half time-step transforms Euler’s method tosymplectic integrator
• more stable over long integrations
• angular momentum is preserved explicitly
• a simple test of the Leapfrog integrator →
Leapfrog Algorithm
• additional half time-step transforms Euler’s method tosymplectic integrator
• more stable over long integrations
• angular momentum is preserved explicitly
• a simple test of the Leapfrog integrator →
So far...
• semi-major axis/ orbital period relationship necessary forresonance
• appropriate integrating scheme
Unresolved...
• Initial conditions for Sun, Jupiter, asteroids
Initial Conditions
• Positions• sun at origin• Jupiter at aphelion• asteroids at perihelion
• Velocities (from r · r)
v2 = µ
[2
r− 1
a
]
Model
• Integrate orbits of the Sun, Jupiter, and five asteroids
• range of initial semi-major axes, e = 0.15
• initial postions• Sun at origin• Jupiter at aphelion• asteroids at perihelion
• calculate eccentricities and semi-major axis
Conclusion
• resonances play a key role
• unite pre-scientific revolution → modern science
• increased computational power → insights into developmentof solar system
References
1 Meteorites may follow a chaotic route to Earth, Wisdom,Nature 315, 731-733 (27 June 1985)
2 The origin of the Kirkwood gaps - A mapping for asteroidalmotion near the 3/1 commensurability, Wisdom, AstronomicalJournal, vol 87, Mar. 1982
3 Numerical Investigation of Chaotic Motion in the AsteroidBelt, Danya Rose, University of Sydney Honours Thesis,November 2008
4 Motion of Asteroids at the Kirkwood Gaps, MakotoYoshikawa, Icarus, Vol. 87, 1990
5 The role of chaotic resonances in the Solar System, N. Murrayand M. Holman, Nature, vol. 410, 12 April 2001
6 Introduction to Celestial Mechanics, Jean Kovalevsky, D.Reidel, 1967
7 Classical Mechanics, John R. Taylor