General Motion Rest: Quasars Linear: Stars Keplerian: Binary Perturbed Keplerian: Asteroids,...
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Transcript of General Motion Rest: Quasars Linear: Stars Keplerian: Binary Perturbed Keplerian: Asteroids,...
General Motion
Rest: Quasars
Linear: Stars
Keplerian: Binary
Perturbed Keplerian: Asteroids, Satellites
Complex: Planets, Space Vehicles
Rotational: Earth, Moon, Satellites, …
Linear Motion
Radial Motion
Proper Motion = Angular Motion
000 ttt vxx
sin
sincos
coscos
rx 0
0
0
0
tt
Vrr R
Quasar/Star Catalog
Epoch
Mean Place (at Epoch)
Parallax (at Epoch)
Proper Motion
Radial Velocity
Astrophys. Quantities:Magnitude, Color, …
ICRFnn, HIPPARCOS, FKn, PPM, AGKn
0t 00 ,
0 ,
RV
Keplerian
Two Body Motion under Newtonian Mech.
Gravitational Constant
Elements = 6 Constants of MotionShapeOrientationTiming
xx
32
2
rdt
d
mMG
ea,,, IΩ
T
Units of Mass
SI: kilogram kg
Astronomical: Solar Mass
Newtonian Gravitational Constant
Measurable Quantity = GM
= Body-centric Gravitational ConstantHeliocentric GeocentricSGM EGM
SM
G
Keplerian Elements
Semi-Major Axis: a
Eccentricity: e
Longitude of Ascending Node: Inclination: I
Argument of Pericenter: Epoch of Pericenter Passage: T
Ellipse
Semi-major axis: a
Semi-minor axis: b 12
2
2
2
b
y
a
x
a
b
Eccentricity
Eccentricity: e, Co-Eccentricity: e’
22
22
1' , ea
be
a
bae
ae
F
Orbital Orientation
Euler (3-1-3) Angles of Orbital Plane RF
3 Important DirectionsDeparture Point: X-axis
Ascending Node: N
Pericenter: P
313313 ,, RRRR II
Z
P
N
I
Orbital Plane
Keplerian Orbits
Elliptic: e < 1Planets, Satellites, Binary
Parabolic: e = 1Good Approximation for Comets
Nearly Parabolic: e ~ 1Comets, some peculiar Asteroids
Hyperbolic: e > 1Space Vehicles, Virtual (Change of Origin)
Elements to Position, Velocity
Solve Kepler’s Equation
Time Derivative of E
PV in Orbital RF
Eb
eEa
sin
cos
TtnEeE sin
Ee
nE
cos1
EEb
EEa
cos
sin
Elements to PV (contd.)
Backward Euler Rotation
00
,,
ΩI, 313Rvx
Kepler’s Equation
First Nonlinear Equation in History
Elliptic
Parabolic
Hyperbolic
MEeE sin
PM3
3
HMFFe sinh
Elliptic Kepler’s Equation
Eccentric Anomaly: E
Mean Anomaly: M = n ( t – T )
Kepler’s 3rd Law
True Anomaly: f
MEeE sin
frEb
freEa
sinsin
coscos
32an
Solution of Kepler’s Equation
Reduction of Variable Domain
Newton Method
Ee
EEEeMEf
Ef
EfEEfE
cos1
sincos
'
*
*
0sin MEeEEf
EM 0 0
Initial Guess for Newton Method
Stability Theory
Initial Guess = Upper Bound
Efficient Choice
0'',0'
,00
EfEf
ff
e
eMeM
e
M
fffE
1
,,
1min
,2
,0min ***0
0* Ef
Perturbed Keplerian Orbits
Elements as Functions of Time
Perturbation Theory
Polynomial + Fourier Series
tΛTΩIeaΛ ,,,,,
kkkkk tStC
tΛtΛΛΛ
sincos
2210
Complex Motion
Equation of Motion
Numerical/Analytical Solution
Parameter Fitting to Observational Data
Results = Ephemeris
xx
32
2
rdt
d
Planetary/Lunar EphemeridesNumerical: DE series (NASA/JPL), DE405Analytical: VSOP/ELP (BdL)DE: available at NAO/CC
Fortran/C callable routines + Binary file(s)DE405: 1600-2200, UNIX/Win/MacP/V of Sun+Moon+9planetsBase: PN Eq.Motion + Precision Data + Least Square Fitting (Mass, Init. Cond., etc.)
Other Solar System Bodies: HORIZONSDetails: http://ssd.jpl.nasa.gov/