1) The document discusses concepts related to gravitation including Newton's law of universal gravitation, gravitational potentials and fields, and spherical harmonics.
2) Gravitation potentials can be used to describe the gravitational field generated by point masses or continuous mass distributions, such as a uniform spherical distribution.
3) Spherical harmonics allow the gravitational potential to be expressed as the sum of terms involving associated Legendre functions, enabling description of more complex mass distributions.
2. Table of Content
SOLO
2
Earth Gravitation
Introduction to Gravitation
Gravitation of a Point Mass M (Netwon Gravitation Law)
Gravitation of a Distribution of Mass Defined by the Density ( )Sr
ρ
Gravitation of a Uniform Distribution of Mass
in a Spherical Volume
( )( ).ConstrS =
ρ
Physical Meaning of the Low Degree and Order SHCs
Reference Earth Model
Clairaut's theorem
Mac Cullagh’s Approximation
World Geodetic System (WGS 84)
Reference Ellipsoid
Air Vehicle in Ellipsoidal Earth Atmosphere
References
3. Gravity
Nicolaus Copernicus (1473 – 1543)
“De Revolutionibus Orbium Coelestium”
(On the Revolutions of the Heavenly Spheres”,
Nuremberg 1543)
SOLO
4. Gravity
Kepler’s Laws of Planetary Motion
From 1601 to 1606 Kepler tried to fit various
Geometric Curves to Tycho Brache’s Data on
Mars Orbit. The result is
“Kepler’s Law of Planetary Motion”
Tycho Brahe
(1546-1601)
Johaness Kepler
(1571-1630)
SOLO
5. KEPLER’S LAWS OF PLANETARY MOTION 1609-1619
•FIRST LAW
THE ORBIT OF EACH PLANET IS
AN ELLIPSE, WITH THE SUN AT
A FOCUS.
b
a
•SECOND LAW
THE LINE JOINING THE PLANET
TO THE SUN SWEEPS OUT
EQUAL AREAS IN EQUAL TIME.
a dA
h
dt
2
=
b
•THIRD LAW
THE SQUARE OF THE PERIOD OF
A PLANET IS PROPORTIONAL TO
THE CUBE OF ITS MEAN DISTANCE
FROM THE SUN.
a 2/322
a
GMGM
ab
TP
ππ
==
b
Gravity
SOLO
6. GALILEO GALILEI (1564-1642(
“DISCOURSESANDMATHEMATICALDEMONSTRATIONS
CONCERNINGTWONEWSCIENCES” 1636
THE FIRST TWO CHAPTERS DEAL WITH
STRENGTHOFMATERIALS.
THIS IS ESSENTIALLY THE FIRST NEW SCIENCE.
THE THIRD AND FOURTH SUBJECT IS :
• UNIFORMMOTION WITHCONSTANTACCELERATION
ANDMOTION OFPROJECTILES
•THE LAWOFINERTIA
•THE COMPOSITION OFMOTIONSACCORDINGTO
VECTORADDITION (“GALILEAN TRANSFORMATION”)
AND
•THE STUDY OFUNIFORMLYACCELERATEDMOTION
Gravity
SOLO
7. NEWTON’SLAWSOFMOTION
“THE MATHEMATICAL PRINCIPLES OF NATURAL PHILOSOPHY”1687
• FIRSTLAW
EVERY BODY CONTINUES IN ITS STATE OF REST OR OF UNIFORM MOTION IN
A STRAIGHT LINE UNLESS IT IS COMPELLED TO CHANGE THAT STATE BY
FORCES IMPRESSED UPON IT.
• SECONDLAW
THE RATE OF CHANGE OF MOMENTUM IS PROPORTIONAL
TO
THE FORCE IMPRESSED AND IS IN THE SAME DIRECTION AS
THAT FORCE.
• THIRDLAW
TO EVERY ACTION THERE IS ALWAYS OPPOSED AN EQUAL REACTION.
Gravity
SOLO
8. NEWTON’S LAW OF UNIVERSAL GRAVITATION
ANY TWO BODY ATTRACT ONE ONOTHER WITH A FORCE
PROPORTIONAL TO THE PRODUCT OF THE MASSES AND INVERSLY
PROPORTIONAL TO THE SQUARE OF THE DISTANCE BETWEEN THEM.
THE UNIVERSAL GRAVITATIONAL CONSTANT
INSTANTANEUS PROPAGATION OF THE FORCE ALONG THE DIRECTION BETWEEN THE
MASES (“ACTION AT A DISTANCE”).
M m
Gravity
SOLO
9. THE LAGEOS SATELLITE MONITORS
ITS POSITION RELATIVE TO THE EARTH
USING REFLECTED LIGHT.
THE TORSION BALANCE EXPERIMENTS:
* HENRY CAVENDISH 1797 * RESEARCH GROUP OF UNIVERSITY OF
WASHINGTON, SEATTLE (EOTWASH)
CAVENDISH EXPERIMENTS HAVE NOT BEEN ABLE TO TEST THE GRAVITATIONAL FORCE AT SEPARATIONS
SMALLER THAN A MILLIMETER.
IF THERE ARE n EXTRA DIMENSIONS (TO THE 3 SPACE + 1 TIME) CURLED UP WITH DIAMETERS R, AT SCALES
SMALLER THAN R THE GENERALIZED NEWTON POTENTIAL WILL BE: Rr
r
M
GrV nn <<=+1
)(
Gravity
Henry Cavendish
(1731 – 1810)
Return to Table of Content
SOLO
10. 10
SOLO
Earth Gravitation
Gravitation of a Point Mass M (Netwon Gravitation Law)
SF
SF
SF
SF
SF
FM rrr
rr
rr
rr
Mm
GgmF
−=
−
−
−
−== :2
According to Newton the Gravitation Force of
Point Mass M on the Point mass mF is given by
MF
The acceleration of Mass m due to Gravity is
( ) ( )rrf
r
r
r
M
Grg
=
−= 2
( ) ( ) ( )
r
r
r
rf
r
r
rf
rf
∂
∂
=∇
∂
∂
=∇
Any function of the form has the property that( )rrf
Because of this
1.we can write
2.we have
( ) ( )rUrg
−∇=
( )
( )
( )
( )
( )
( )
( )
( )
( )
( )
( )
( )
( ) ( )[ ]1
1111
rUrUmrUdmrdrUmrdrgmrdrF F
rB
rA
F
rB
rA
rB
rA
rB
rA
−=−=⋅∇−=⋅=⋅ ∫∫∫∫
The Work necessary to move the Mass mF in the Gravity Field of Point Mass M,
from point to point , is not a function of the trajectory chosen but on
the values of the scalar function U (called Potential) at those two points.
( )rA
( )1rB
11. SOLO
11
Earth Gravitation
Gravitation of a Point Mass M (Netwon Gravitation Law)
( ) ( ) ( )
( )
( )
( )
( )
( )
( )
r
M
G
r
M
Grd
r
M
Grd
r
r
r
M
GrdrgrUrU
f
rB
rA
rB
rA
rB
rA
f
fff
−=−=⋅
−=⋅=− ∫∫∫ 22
The Gravitation Potential U of a Point Mass M is given by
The Gravitation Equi-Potential Surface of a Point Mass M
is Spherical Surface centered at M location.
Gravitation of a Distribution of Mass Defined by the Density ( )Sr
ρ
The Gravitation Potential of the Distribution is obtaining by
Integrating the Gravitation Potentials of the Point Masses dm
over the Volume V
( ) ( ) ( )
∫∫ −
−=
−
−=
V
S
S
S
M S
S
Vd
rr
r
G
rr
rmd
GrU
ρ
If we take the reference rf → ∞ we get 0. ==
fr
M
GConst
( )
r
M
GrU
−=
( ) .Const
r
M
GrU +−=
Return to Table of Content
12. SOLO
12
Earth Gravitation
( ) S
SS
S
rrMd
r
r
r
rr
G
rr
Md
GrUd >
+
−
−=
−
−=
2
cos21
1
γ
( ) ( ) SSSSSSSS
onDistributi
Density
SSS ddrdrrVdrMd ϕθθθϕρθϕρ sin,,,,
2
==
( ) ( )
S
r
SS
SSSSSSSS
rr
r
r
r
r
ddrdrr
r
G
rU
S S S
>
+
−
−= ∫ ∫∫ϕ θ
γ
ϕθθθϕρ
2
2
cos21
sin,,
( ) S
n
n
n
SSS
rrP
r
r
r
r
r
r
>
=
+
− ∑
∞
=
−
0
2/12
coscos21 γγ
Pn (u) are Lagrange Polynomials, of order n, given explicitly by Rodrigues’ Formula:
( ) ( )
n
nn
kn
ud
ud
n
uP
1
!2
1 2
−
=
Gravitation of a Distribution of Mass Defined by the Density ( )Sr
ρ
( ) ( ) ( ) ( ) 2/13&,1 2
210 −=== uuPuuPuPExamples:
Using Spherical Coordinates (rS, φS, θS)
The Potential Differential of any distribution of mass is given by:
13. SOLO
13
Earth Gravitation
( ) ( ) ( ) S
r Md
SSSSSSSS
n
n
n
S
rrddrdrrP
r
r
r
G
rU
S S S
>
−= ∫ ∫ ∫ ∑
∞
=ϕ θ
ϕθθθϕργ
sin,,cos
2
0
From Spherical Trigonometry:
( )SSS ϕϕθθθθγ −+= cossinsincoscoscos
According to Addition Theorem for Spherical Harmonics:
( ) ( ) ( ) ( )
( )
( )[ ] ( ) ( )∑=
−
+
−
+=
n
m
S
m
n
m
nSSnnn PPm
mn
mn
PPP
1
coscoscos
!
!
2coscoscos θθϕϕθθγ
( ) ( ) ( )uP
ud
d
uuP nm
m
mm
n
2/2
1: −=
Where Pn
m
(u) is the Associated Lagrange Function of the First Kind of Degree n
and Order m, given by:
Gravitation of a Distribution of Mass Defined by the Density ( )Sr
ρ
( ) ( )uPuP nn =
0
( ) ( ) ( ) ( )22
2
2
1
21
2 13,13 ttPtttP −=−=They satisfy:
The Potential of any distribution of mass is given by:
See Presentation on
“Legendre Functions”
14. SOLO
14
Earth Gravitation
The Potential of any distribution of mass is given by:
( ) ( ) ( )
( ) ( ) S
n r Md
SSSSSSSSn
n
S
k
S
r Md
SSSSSSSS
k
n
n
S
rrddrdrrP
a
r
r
a
r
G
rrddrdrrP
r
r
r
G
rU
S S S
S S S
>
−=
>
−=
∑ ∫ ∫∫
∫ ∫∫ ∑
∞
=
∞
=
0
2
2
0
sin,,cos
sin,,cos
ϕ θ
ϕ θ
ϕθθθϕργ
ϕθθθϕργ
According to Addition Theorem for Spherical Harmonics:
( ) ( ) ( ) ( )
( )
( )[ ] ( ) ( )∑=
−
+
−
+=
n
m
S
m
n
m
nSSnnn PPm
mn
mn
PPP
1
coscoscos
!
!
2coscoscos θθϕϕθθγ
Using those results we obtain:
( ) 1cos0 =γP
( ) ( ) ( ) ( ) ( ) ( )
( )
( )
( ) ( ) ( ) ( ) ( )
( )
( )
( ) ( ) ( ) ( ) ( )∑ ∫ ∫ ∫
∑∑ ∫ ∫∫
∑ ∫ ∫ ∫∫ ∫ ∫
∞
=
∞
= =
∞
=
+
−
−
+
−
−
−
−=
1
2
1 0
2
1
22
1
0
0
sin,,sincossincos
!
!
2
sin,,coscoscoscos
!
!
2
sin,,coscossin,,cos
n r
SSSSSSSSSSn
n
S
n
n
n
n
m r
SSSSSSSSSS
m
n
n
Sm
n
n
n r
SSSSSSSSSn
n
S
n
n
M
r Md
SSSSSSSS
S
S S S
S S S
S S SS S S
ddrdrrmP
a
r
mP
r
a
mn
mn
r
G
ddrdrrmP
a
r
mP
r
a
mn
mn
r
G
ddrdrrP
a
r
P
r
a
r
G
ddrdrrP
a
r
r
G
rU
ϕ θ
ϕ θ
ϕ θϕ θ
ϕθθθϕρϕθϕθ
ϕθθθϕρϕθϕθ
ϕθθθϕρθθϕθθθϕργ
Gravitation of a Distribution of Mass Defined by the Density ( )Sr
ρ
a – any reference length
15. SOLO
15
Earth Gravitation
( ) ( ) ( ) ( ) ( )( )
+
+
+−= ∑∑∑
∞
= =
∞
= 1 11
0 sincoscoscos1
n
n
m
nmnm
m
n
n
n
nn
n
mSmCP
r
a
CP
r
a
r
MG
rU ϕϕθθ
( ) ( )∫∫∫
==
S S Sr Md
SSSSSSSSSn
n
S
nn ddrdrrP
a
r
M
CC
ϕ θ
ϕθθθϕρθ
sin,,cos
1
:
2
0
( )
( )
( )
( )
( )
( )∫ ∫∫
+
−
=
S S Sr Md
SSSSSSSS
S
S
S
m
n
n
S
nm
nm
ddrdrr
m
m
P
a
r
mn
mn
S
C
ϕ θ
ϕθθθϕρ
ϕ
ϕ
θ
sin,,
sin
cos
cos
!
!
2:
2
Gravitation of a Distribution of Mass Defined by the Density ( )Sr
ρ
The Potential of any distribution of mass is given by:
16. SOLO
16
Earth Gravitation
(1) A tremendous simplification results if the mass
distribution is symmetric about the z axis, i.e. ρ is a
function only of rS and θS. Since
( ) ( ) ,2,10cossin
2
0
2
0
=== ∫∫ jdjdj SSSS
ππ
ϕϕϕϕ
the coefficients Cmn and Smn vanish identically.
(2) In addition to axial symmetry, the origin of coordinates coincides with the
center of mass, the constant C1 is identically zero.
( ) ( ) 0cos
1
sin,cos
1
:
2
cos
11 =
=
= ∫∫ ∫∫ m
S
S
r md
SSSSSSSS
S
md
a
r
M
ddrdrrP
a
r
M
C
S S S
S
θϕθθθρθ
ϕ θ θ
C1 is proportional to the first moment of the mass M with respect to the xy plane.
Gravitation of a Distribution of Mass Defined by the Density ( )Sr
ρ
In this case
( ) ( ) 0
1
:cos1 nn
n
nn
n
CJJP
r
a
r
MG
rU −=
−−= ∑
∞
=
θ
17. SOLO
17
Earth Gravitation
(3) Finally, if the mass is distributed in homogeneous concentric layers, i.e. ρ is a
function only of rS , then Cn vanishes identically for all n
( ) ( ) 0sincos:
2
0
0
00
22
=
= ∫∫∫
+ ππ
ϕθθθρ SSSSk
R
SS
n
S
n ddPrdr
a
r
M
a
C
Gravitation of a Distribution of Mass Defined by the Density ( )Sr
ρ
( )
r
MG
rU =
In this case
Return to Table of Content
18. SOLO
18
Earth Gravitation
Gravitation of a Uniform Distribution of Mass in a Spherical Volume( )( ).ConstrS =
ρ
For a Static Spherical Volume with an Uniform Distributed
Mass the Gravitation Potential at a distance r > R is given by
( )
r
MG
r
R
GVd
rr
GrU S
V
S
SS
−=−=
−
−= ∫
3/41 3
π
ρρ
The Gravitation Potential for a Static Spherical Volume with
an Uniform Distributed Mass is equivalent to a Point Mass
Gravitation Potential concentrated at the Center of the
Sphere. The Equi-Potential Surfaces will be Concentric
Spherical Surfaces outside the Spherical Mass.
19. SOLO
19
Earth Gravitation
The Potential of the Reference Ellipsoid is given by:
where:
UG – Gravitational Potential (m2
/s2
)
GM – Earth’s Gravitational Constant
r - Distance from the Earth’s Center of Mass
rS - Distance from the Earth’s Center of Mass to d m
Gravitation of a Uniform Distribution of Mass in a Ellipsoid Volume( )( ).Constr =
ρ
( )
Srr
md
GrUd
−
=
Typically the Potential is expanded in a series.
This can be done in two ways, which lead to the same
result:
1.By expanding the term and integrate the result
term by term.
2. By writing the Potential as solution of Lalace’s
Equation using Spherical Harmonics.
Srr
−
1
20. SOLO
20
Earth Gravitation
The Potential Equation of Gravity Field
where:
UG – Gravitational Potential (m2
/s2
)
GM – Earth’s Gravitational Constant
r - Distance from the Earth’s Center of Mass
rS - Distance from the Earth’s Center of Mass to dm
( ) ( )
( ) ( )
( )rG
VdrrrG
Vd
rr
rGrU
S
S
V
SSS
V
S
S
SS
ρπ
δπρ
ρ
4
4
122
−=
−−=
−
∇−=∇
∫∫∫
∫∫∫
( ) ( )∫∫∫∫ −
−=
−
−=
SV S
S
S
M S rr
Vd
rG
rr
md
GrU
ρStart with:
Inside the mass M we have:
( ) ( )rGrU
ρπ42
−=∇Poisson Equation:
( ) 02
=∇ rU
Laplace Equation:
Outside the mass M we have:
Siméon Denis
Poisson
1781-1840
Pierre-Simon Laplace
(1749-1827)
Return to Table of Content
21. SOLO
21
Earth Gravitation
Physical Meaning of the Low Degree and Order SHCs
Gravitation of a Distribution of Mass Defined by the Density ( )Sr
ρ
As pointed out in the previous slides the first term of the
Spherical Harmonic Coefficients (SHC) of Gravity
Potential is equal to the Potential for Spherical Mass. The
remaining terms then represent the Gravitational Potential
due to Non-spherical, Non-uniform Mass.
( ) ( ) ( ) ( ) ( )( )
+
+
+−= ∑∑∑
∞
= =
∞
= 1 11
0 sincoscoscos1
n
n
m
nmnm
m
n
n
n
nn
n
mSmCP
r
a
CP
r
a
r
MG
rU ϕϕθθ
We have (see Figure)
=
=
S
SS
SS
S
s
s
s
S r
z
y
x
r
θ
ϕθ
ϕθ
cos
sinsin
cossin
( ) 0&
1
cos
1
: 10
cos
1
1
110 ===
== ∫∫ S
a
z
Mdz
Ma
MdP
a
r
M
CC G
M
S
M
S
S
S
θ
θ
( )
=
=
=
=
∫∫ ∫ ay
ax
Md
y
x
Ma
Md
a
r
M
MdP
a
r
MS
C
G
G
M S
S
M M S
S
S
S
S
S
S
S
/
/
2
2
sin
cos
sin
2
sin
cos
cos
2
1
1
1
1
11
11
ϕ
ϕ
θ
ϕ
ϕ
θ
( ) ( )2
1
21
1 1 ttP −=where we used Legendre Polynomials.
GGG zyx
,, are the coordinates of the Mass Center of Gravity
22. SOLO
22
Earth Gravitation
Physical Meaning of the Low Degree and Order SHCs
Gravitation of a Distribution of Mass Defined by the Density ( )Sr
ρ
( ) ( ) ( ) ( ) ( )( )
+
+
+−= ∑∑∑
∞
= =
∞
= 1 11
0 sincoscoscos1
n
n
m
nmnm
m
n
n
n
nn
n
mSmCP
r
a
CP
r
a
r
MG
rU ϕϕθθ
=
=
S
SS
SS
S
s
s
s
S r
z
y
x
r
θ
ϕθ
ϕθ
cos
sinsin
cossin
+
−−=
−=
2
1
2
31
2220
SSSS
SSSSSS
yyxx
zzzzrr
II
I
Ma
II
Ma
C
( )∫
=
M
S
S
MdP
a
r
MS
C
0
1
cos
2 0
2
2
20
20
θ
( ) ( )
+
−++=
+
−=
−−−
=
−
==
2
3
1
2
1
2
3
2
1cos3
coscos
2
222
2
22
2
22
22222
2
2
22
2
0
22
2
SS
SSS
SS
S
SSSSSS
S
S
S
S yx
zyx
a
yx
z
aa
zyxz
a
r
P
a
r
P
a
r θ
θθ
( ) ∫∫∫
=
=
=
=
M zy
zx
SS
SS
M S
S
SSS
M S
S
S
S
MaI
MaI
Md
zy
zx
Ma
Mdr
Ma
MdP
a
r
MS
C
SS
SS
2
2
2
2
2
1
2
2
21
21
/
/1
sin
cos
cossin3
3
1
sin
cos
cos
!3
12
ϕ
ϕ
θθ
ϕ
ϕ
θ
( )
( ) ( )
( )∫∫∫
−
=
−
=
−
⋅
=
=
M yx
xxyy
SS
SS
M SS
SS
SS
M S
S
S
S
MaI
MaII
Md
yx
yx
Ma
Mdr
Ma
MdP
a
r
MS
C
SS
SSSS
2
222
2
22
22
2
2
2
2
22
22
2/
4/
24
1
cossin2
sincos
sin3
34
1
2sin
2cos
cos
!4
!12
ϕϕ
ϕϕ
θ
ϕ
ϕ
θ
( ) ( ) ( ) ( )22
2
2
1
21
2 13,13 ttPtttP −=−=where we used
( ) ( ) ( ) ( ) ( )SSSSSSSSSSSSSS zzyyxx
M
SSSrr
M
SSzz
M
SSyy
M
SSxx IIIMdzyxIMdyxIMdzxIMdzyI ++=++=+=+=+= ∫∫∫∫ 2
1
::,:,:
222222222
Define Moments of Inertia
24. SOLO
24
Earth Gravitation
Physical Meaning of the Low Degree and Order SHCs
Gravitation of a Distribution of Mass Defined by the Density ( )Sr
ρ
Return to Table of Content
25. SOLO
25
Earth Gravitation
Earth is a Rotating Non-Spherical Body, with a slightly non-
uniform mass distribution. The force acting on an external
mass is due to Gravitation and Centrifugal Accelerations.
To find a Model for the Gravitation Acceleration the Earth
is approximated by an Ellipsoid
The flattering of the Earth was already discovered by the end of the 18th
century.
It was noticed that the distance between a degree of Latitude as measured, for
instance with a sextant, differs from that expected from a Sphere:
RE (θ1 – θ2) ≠ RE dθ, with RE the radius of the Earth, θ1 and θ2 two different
Latitudes
f - the flattening of a meridian
section of the Earth, defined as:
a
ba
f
−
=:
R = 6,371.000 km
a = 6,378.136 km
b = 6,356.751 km
Reference Earth Model
Return to Table of Content
26. SOLO
26
Reference Ellipsoid
Meridian Ellipse Equation: 12
2
2
2
=+
b
z
a
p
Slope of the Normal to Ellipse:
2
2
tan
bp
az
zd
pd
=−=φ
The Slope of the Geocentric Line to the same point
p
z
O =φtan OO RzRp φφ sincos ==
Deviation Angle between Geographic and Geodetic
At Ellipsoid Surface
O
b
a
φφ tantan 2
2
=
= −
O
b
a
φφ tantan 2
2
1
( ) ( ) φφφφ tan1tan1tantan
22
2
2
fe
a
b
O −=−==
a
ba
f
−
=:
2
2
22
2
2: ff
a
ba
e −=
−
=
Earth Gravitation
27. SOLO
27
Reference Ellipsoid
Meridian Ellipse Equation:
Oφφδ −=
12
2
2
2
=+
b
z
a
p
Slope of the Normal to Ellipse:
2
2
tan
bp
az
zd
pd
=−=φ
The Slope of the Geocentric Line to the same point
p
z
O =φtan
−=
−+
−
=
+
−
=
+
−
= 1
11
1
1
tantan1
tantan
tan 2
2
2
2
2
2
2
2
2
22
22
2
2
b
a
a
zp
a
p
p
a
b
a
p
z
bp
az
p
z
bp
az
O
O
φφ
φφ
δ
OO RzRp φφ sincos ==
( )
( ) ( )OO
f
O f
ba
R
b
ba
a
ba
R
ba
ba
φφφδ 2sin2sin
2
tan2sin
2
tan
1
2
11
12
22
22
1
≈
+
−
=
−
=
≈≈<<
−−
Deviation Angle between Geographic and Geodetic
At Ellipsoid Surface
Earth Gravitation
28. SOLO
28
Reference Ellipsoid
For a point at a Height h near the Ellipsoid the
value of δ must be corrected:
u−= 1δδ
From the Law of Sine we have:
Deviation Angle between Geographic and Geodetic
At Altitude h from Ellipsoid Surface
( ) R
h
hR
huu
≈
+
≈=
− 11 sin
sin
sin
sin
δδπ
Since u and δ1 are small: 1δ
R
h
u ≈
The corrected value of δ is:
( )Of
R
h
R
h
u φδδδ 2sin11 11
−=
−=−=
Therefore:
( )OO f
R
h
φλδφφ 2sin1
−+=+=
Earth Gravitation
29. SOLO
29
World Geodetic System (WGS 84)
where
λ – Longitude
e – Eccentricity = 0.08181919
Reference Earth Model
In Earth Center Earth Fixed Coordinate –ECEF-System (E)
the Vehicle Position is given by:
( )
( )
( )
( )
+
+
+
=
=
φ
φλ
φλ
sin
cossin
coscos
HR
HR
HR
z
y
x
P
M
N
N
E
E
E
E
( )
NhH
e
a
RN
+=
−
= 2/12
sin1 φ
Another variable, used frequently, is the radius of the
Ellipsoid referred as the Meridian Radius
( )
( ) 2/32
2
sin1
1
φe
ea
RM
−
−
=
Earth Gravitation
30. SOLO
30
Reference Ellipsoid
b
a
Oφ
?O – Geographic Latitude
? – Geodetic Latitude
Equator
North Pole
Tangent
to Ellipsoid
p
NR
z
P
a
r
φ
β
Meridian Ellipse
Ellipsoid Equation:
( ) 222
2
2
2
22
11 aeb
b
z
a
yx
−==+
+
Define: 22
: yxp +=
12
2
2
2
=+
b
z
a
p
Differentiate: 022
=+
b
dzz
a
dpp
z
p
a
b
dp
dz
2
2
cot =−=φFrom the Figure:
φtan2
2
p
a
b
z =
( )φφ 222
4
2
22
4
2
2
2
tantan1 ba
a
p
p
a
b
a
p
+=+=
φφ
φ
φφ
φ
2222
2
2222
2
sincos
sin
,
sincos
cos
ba
b
z
ba
a
p
+
=
+
=
Earth Gravitation
32. SOLO
32
Reference Ellipsoid
( ) 222
1 aeb −=
12
2
2
2
=+
b
z
a
p
0
0
sin
cos
φ
φ
rz
rp
=
=
1
sincos
2
0
2
2
0
2
2
=
+
ba
r
φφ
( )
2/1
2
0
2
2
0
2
0
sincos
−
+=
ba
r
φφ
φ
( )
( ) ( )0
22/1
0
2
2/1
0
2
2
2/1
0
2
2
222/1
0
2
2
2
0
2
0
sin1sin21
sin1sin1sincos
φφ
φφφφφ
fafa
b
ba
b
a
a
ba
a
b
ba
a
b
a
ar
f
−≈+≈
+−
+=
−
+=
+=
−
−
≈
−−
Earth Gravitation
33. SOLO
33
Reference Ellipsoid
The Meridians and Parallels are the Lines of Curvature of the
Ellipsoid. The principal Radii of Curvature are therefore in
the Plane of Meridian (Meridian Radius of Curvature RM) and
in the Plane of Prime Vertical, perpendicular to Meridian
Plane (Radius of Curvature in the Prime Vertical RN)
Radiuses of Curvature of the Ellipsoid
Meridian Ellipse Equation: ( ) 222
2
2
2
2
11 aeb
b
z
a
p
−==+
From this Equation, at any point (x,y) on the Ellipse, we have:
φtan
1
2
2
−=−=
az
bp
pd
zd
32
4
32
2222
2
2
2
2
22
2
22
2
2
2
111
za
b
za
pbza
a
b
z
p
a
b
z
p
za
b
pd
zd
z
p
za
b
pd
zd
−=
+
−=
+−=
−−=
From the Ellipse Equation:
( ) φ
φ
φ 2
22
2
2
2
222
2
2
2
2
2
2
2
2
cos
sin1
1
1
tan1111
e
a
p
e
e
a
p
b
a
p
z
a
p −
=
−
−+=
+=
( )
( )
( ) 2/122
2
2
2
2/122
sin1
sin1
tan
sin1
cos
φ
φ
φ
φ
φ
e
ea
p
a
b
z
e
a
p
−
−
==→
−
=
From the Figure on right:
( ) 2/122
sin1cos φφ e
ap
RN
−
==
Earth Gravitation
34. SOLO
34
Reference Ellipsoid
Let develop the RN and RM (continue):
we have at any point (p,z) on the Ellipse:
φtan
1
2
2
−=−=
az
bp
pd
zd ( )
3
22
32
4
2
2
11
z
ea
za
b
pd
zd −
−=−=
The Radius of Curvature of the Ellipse at the
point (p,z) is:
( )
( )
( )
( )
( ) 2/322
2
2/322
3323
22
2/3
2
2
2
2/32
sin1
1
sin1
sin1
1
tan
1
11
:
φφ
φφ
e
ea
e
ea
ea
pd
zd
pd
zd
RM
−
−
=
−
−
−
+
=
+
=
( )
( )
( ) 2/122
2
2/122
sin1
sin1
sin1
cos
φ
φ
φ
φ
e
ea
z
e
a
p
−
−
=
−
=
( )
( ) 2/322
2
sin1
1
:
φe
ea
RM
−
−
=
Radiuses of Curvature of the Ellipsoid
Earth Gravitation
35. SOLO
35
Reference Ellipsoid
( )
( ) 2/322
2
sin1
1
:
φe
ea
RM
−
−
=
( ) 2/122
sin1cos φφ e
ap
RN
−
==
a
ba
f
−
=: 2
2
22
2
2: ff
a
ba
e −=
−
=Using
( )
( )[ ]
( ) ( ) [ ] ++−≈
+−++−≈
−−
−
= φφ
φ
2222
2/322
2
sin321sin2
2
3
121
sin21
1
: ffaffffa
ff
fa
RM
( )[ ]
( ) [ ]φφ
φ
222
2/122
sin31sin2
2
3
1
sin21
faffa
ff
a
RN +≈
+−+≈
−−
=
[ ]φ2
sin321 ffaRM +−≈
[ ]φ2
sin31 faRN +≈
We used and we neglect f2
terms
( )
( ) +
−
++=
− !2
1
1
1
1 nn
xn
x
n
Radiuses of Curvature of the Ellipsoid
Return to Table of Content
Earth Gravitation
36. SOLO
36
Reference Earth Model
Clairaut's theorem
Clairaut's theorem, published in 1743 by Alexis Claude Clairaut in
his “Théorie de la figure de la terre, tirée des principes de
l'hydrostatique”, synthesized physical and geodetic evidence that
the Earth is an oblate rotational ellipsoid. It is a general
mathematical law applying to spheroids of revolution. It was
initially used to relate the gravity at any point on the Earth's
surface to the position of that point, allowing the ellipticity of the
Earth to be calculated from measurements of gravity at different
latitudes.
Clairaut's formula for the acceleration due to gravity g on the surface of a spheroid
at latitude , was:ϕ
where G is the value of the acceleration of gravity at the equator, m the ratio of
the centrifugal force to gravity at the equator, and f the flattening of a meridian
section of the earth, defined as:
a
ba
f
−
=:
Alexis Claude Clairaut
)1713–1765(
−+= φ2
sin
2
5
1 fmGg
Earth Gravitation
Return to Table of Content
37. SOLO
37
Reference Earth Model
Mac Cullagh’s Approximation (1845)
James MacCullagh
(1809 – 1847)
Mac Cullagh’s used the Approximation:
( )
( )
( )
( ) ( )
−
−
+
+−≈ ∫∫
≈
M
P
SS
P
r
a
M
M P
S
S
P
Md
a
r
Mr
a
Md
a
r
Mr
a
M
r
G
rU
S
CM
S
θθ
θ
θ
θθ
θθ
cos
22
cos
22
cos
1
cos
1
22
0
1
1
2
1cos31
2
1cos3
cos
1
cos1
∫∫∫
+
−++=
+
−=
−
=
M
SS
SSS
M
SS
S
M
SS
dM
yx
zyx
Ma
dM
yx
z
Ma
dM
a
r
M
C
2
3
1
2
1
2
1cos31
:
2
222
2
22
2
2
2
2
2
20
θ
222220
2
1
2
31
J
Ma
ACII
I
Ma
II
Ma
C SSSS
SSSSSS
yyxx
zzzzrr −=
−
−=
+
−−=
−=
( ) ( ) ( ) ( ) ( )SSSSSSSSSSSSSS zzyyxx
M
SSSrr
M
SSzz
M
SSyy
M
SSxx IIIMdzyxIMdyxIMdzxIMdzyI ++=++=+=+=+= ∫∫∫∫ 2
1
::,:,:
222222222
Define Moments of Inertia
2
:,: SSSS
SS
yyxx
zz
II
AIC
+
==
( )
( )
Ma
AC
JJ
r
aMG
M
r
G
rU
P
22
2
23
2
:
2
1cos3
2
−
=
−
+−≈
θ
θ
Earth Gravitation
Return to Table of Content
38. SOLO
38
Reference Earth Model
The definition of geodetic latitude (φ) and
longitude (λ) on an ellipsoid. The normal
to the surface does not pass through the
centre
Reference Ellipsoid
Geodetic latitude: the angle between the
normal and the equatorial plane. The
standard notation in English publications is ϕ
Geocentric latitude: the equatorial plane and
the radius from the centre to a point on the
surface. The relation between the geocentric
latitude (ψ) and the geodetic latitude ( ) isϕ
derived in the above references as
The definition of geodetic (or
geographic) and geocentric latitudes
( ) ( )[ ]φφψ tan1tan 21
e−= −
To use previous results, where we used
spherical coordinates, rS, φS, θS we will use
θ
π
ψϕλ −==
2
&
Earth Gravitation
39. SOLO
39
Earth Gravitation
Centrifugal Potential
Since Earth is a Rotating Body, a Centrifugal Acceleration is
exerted on a Mass m, at a (x,y,z) Position, given by
( ) Cyx
yxV
yx
C Uyx
yx
yx
Va ∇=+Ω=
+
+
Ω=
+Ω=
11
11 2
22
22
where:
Ω = 7292115.1467x10-11
rad/s – Earth Angular Velocity
The Centrifugal Earth Potential UC at (x,y,z) Position is
given by
( ) ( )
( ) .
.1111..
2
2
Constydyxdx
ConstydxdyxConstrdUConstUdU yxyxCCC
++Ω=
++⋅+Ω=+⋅∇=+=
∫∫
∫∫∫
Centrifugal Potential
Earth Gravitation Model
( )222
2
1
yxUC +Ω=
By choosing Const. = 0, we obtain
40. SOLO
40
Earth Gravitation
Potential of the Rotating Reference Ellipsoid
The Potential of the Rotating Reference Ellipsoid is the sum of the Gravitational and
Centrifugal Potentials:
CG UUW +=
( ) .
2
1 222
ConstyxUC ++Ω=
The Gravitational Potential of the Reference Ellipsoid
(assuming Uniform Density Distribution) is:
( ) ( )
+
+−= ∑∑= =
max
2 0
sincossin1
n
n
n
m
nmnmnm
n
G mSmCP
r
a
r
MG
U λλψ
where:
UG – Gravitational Potential (m2
/s2
)
GM – Earth’s Gravitational Constant
r - Distance from the Earth’s Center of Mass
a - Semi-Major Axis of the WG 84 Ellipsoid
n,m – Degree and Order respectively
ψ– Geocentric Latitude
λ – Geocentric Longitude = Geodetic Longitude Return to Table of Content
41. SOLO
41
Earth Gravitation
The WGS 84 Gravity Model is defined in terms of normalized coefficients:
( ) ( ) ( ) ( ) ( )( )
+
+
+−= ∑∑∑
∞
= =
∞
= 1 11
0 sincossinsin1
n
n
m
nmnm
m
n
n
n
nn
n
mSmCP
r
a
CP
r
a
r
MG
rU λλψψ
( )∫
==
M
Sn
n
S
nn MdP
a
r
M
CC ψsin
1
:0
( )
( )
( )
( )
( )∫
+
−
=
M S
S
S
m
n
n
S
nm
nm
Md
m
m
P
a
r
mn
mn
S
C
λ
λ
ψ
sin
cos
sin
!
!
2:
( ) ( ) ( ) ( ) ( )( )
+
+
+−= ∑∑∑
∞
= =
∞
= 1 11
0 sincossinsin1
n
n
m
nmnm
m
n
n
n
nn
n
mSmCP
r
a
CP
r
a
r
MG
rU λλψψ
( ) ( ) ( )
( )
( )
≠
=
=
+
−
+=
02
01
sin
!
!
12sin
m
m
kP
mn
mn
knP
m
n
m
n ψψ
( )
( )
( )
≠
=
=
−
+
+
=
02
01
!
!
12
1
m
m
k
S
C
mn
mn
knS
C
nm
nm
nm
nm
Cnm and Snm are called Spherical Harmonic Coefficients (SHC).
The Gravitation Potential of the Earth Model is given by:
Earth Gravitation Model
World Geodetic System (WGS 84)
42. SOLO
42
World Geodetic System (WGS 84)
Reference Earth Model
Spherical Harmonics
Visual representations of the first few
spherical harmonics. Red portions represent
regions where the function is positive, and
green portions represent regions where the
function is negative.
Earth Gravitation
43. SOLO
43
World Geodetic System (WGS 84)
Reference Earth Model
Carlo Somigliana
(1860 –1955)
The Theoretical Gravity on the surface of the Ellipsoid
is given by the Somigliana Formula (1929)
84
22
2
2222
22
sin1
sin1
sincos
sincos
WGS
e
pe
e
k
ba
ba
φ
φ
γ
φφ
φγφγ
γ
−
+
=
+
+
=
where
1: −=
e
p
a
b
k
γ
γ
2
22
:
a
ba
e
−
= - Ellipsoid Eccentricity
a - Ellipsoid Semi-major Axis = 6378137.0 m
b - Ellipsoid Semi-minor Axis = 6356752.314 m
γp – Gravity at the Poles = 983.21849378 cm/s2
γe – Gravity at the Equator = 978.03267714 cm/s2
– Geodetic Latitudeϕ
The Theory of the Equipotential Ellipsoid was first given by
P. Pizzetti (1894)
Earth Gravitation
44. SOLO
44
World Geodetic System (WGS 84)
Reference Earth Model
The coordinate origin of WGS 84 is meant to be located at the
Earth's center of mass; the error is believed to be less than 2 cm.
The WGS 84 meridian of zero longitude is the IERS Reference
Meridian. 5.31 arc seconds or 102.5 meters (336.3 ft) east of the
Greenwich meridian at the latitude of the Royal Observatory.
The WGS 84 datum surface is an oblate spheroid (ellipsoid) with major
(transverse) radius a = 6378137 m at the equator and flattening
f = 1/298.257223563.The polar semi-minor (conjugate) radius b then equals a
times (1−f), or b = 6356752.3142 m.
Presently WGS 84 uses the EGM96 (Earth Gravitational Model 1996) Geoid,
revised in 2004. This Geoid defines the nominal sea level surface by means of a
spherical harmonics series of degree 360 (which provides about 100 km
horizontal resolution).[7]
The deviations of the EGM96 Geoid from the WGS 84
Reference Ellipsoid range from about −105 m to about +85 m.[8]
EGM96 differs
from the original WGS 84 Geoid, referred to as EGM84.
Earth Gravitation
46. SOLO
46
World Geodetic System (WGS 84)
Reference Earth Model
Geoid product, the 15-minute, worldwide Geoid Height for EGM96
The difference between the Geoid and the Reference Ellipsoid exhibit the
following statistics:
Mean = - 0.57 m, Standard Deviation = 30.56 m
Minimum = -106.99 m, Maximum = 85.39 m
Earth Gravitation
47. SOLO
47
World Geodetic System (WGS – 84)
Reference Earth Model
Parameters Notation Value
Ellipsoid Semi-major Axis a 6.378.137 m
Ellipsoid Flattening (Ellipticity) f 1/298.257223563
(0.00335281066474)
Second Degree Zonal Harmonic Coefficient of the Geopotential C2,0 -484.16685x10-6
Angular Velocity of the Earth Ω 7.292115x10-5
rad/s
The Earth’s Gravitational Constant (Mass of Earth includes
Atmosphere)
GM 3.986005x1014
m3
/s2
Mass of Earth (Includes Atmosphere) M 5.9733328x1024
kg
Theoretical (Normal) Gravity at the Equator (on the Ellipsoid) γe 9.7803267714 m/s2
Theoretical (Normal) Gravity at the Poles (on the Ellipsoid) γp 9.8321863685 m/s2
Mean Value of Theoretical (Normal) Gravity γ 9.7976446561 m/s2
Geodetic and Geophysical Parameters of the WGS-84 Ellipsoid
Earth Gravitation
48. SOLO
48
World Geodetic System (WGS 84)
Reference Earth Model
a
ba
f
−
=:f - Ellipsoid Flattening (Ellipticity)
a - Ellipsoid Semi-major Axis
b - Ellipsoid Semi-minor Axis
e - Ellipsoid Eccentricity 2
2
22
2
2: ff
a
ba
e −=
−
=
( ) 2
11 eafab −=−=
Reference Ellipsoid
Earth Gravitation
49. SOLO
49
World Geodetic System (WGS 84)
where
λ – Longitude
e – Eccentricity = 0.08181919
Reference Earth Model
In Earth Center Earth Fixed Coordinate –ECEF-System (E)
the Vehicle Position is given by:
( )
( )
( )
( )
+
+
+
=
=
φ
φλ
φλ
sin
cossin
coscos
HR
HR
HR
z
y
x
P
M
N
N
E
E
E
E
( )
NhH
e
a
RN
+=
−
= 2/12
sin1 φ
Another variable, used frequently, is the radius of the
Ellipsoid referred as the Meridian Radius
( )
( ) 2/32
2
sin1
1
φe
ea
RM
−
−
=
Radius of Curvature in the Prime
Vertical
Return to Table of Content
Earth Gravitation
51. 51
SOLO
7. Forces Acting on the Vehicle (continue – 4)
Gravitation Acceleration
( ) ( )
−
−
−
==
zg
yg
xg
gg
100
0
0
0
010
0
0
0
001
χχ
χχ
γγ
γγ
σσ
σσ cs
sc
cs
sc
cs
scC EW
E
W
( )
gg
−
=
γσ
γσ
γ
cc
cs
s
W
2sec/174.322sec/81.9
0
2
0
0
0
gg ftmg
HR
R
==
+
=
The derivation of Gravitation Acceleration assumes an Ellipsoidal Symmetrical Earth.
The Gravitational Potential U (R, ) is given byϕ
( ) ( )
( )
( )φ
φ
µ
φ
,
sin1, 2
RUg
P
R
a
J
R
RU
E
E
n n
n
n
∇=
−⋅−= ∑
∞
=
μ – The Earth Gravitational Constant
a – Mean Equatorial Radius of the Earth
R=[xE
2
+yE
2
+zE
2
]]/2
is the magnitude of
the Geocentric Position Vector
– Geocentric Latitude (sin =zϕ ϕ E/R)
Jn – Coefficients of Zonal Harmonics of the
Earth Potential Function
P (sin ) – Associated Legendre Polynomialsϕ
Air Vehicle in Ellipsoidal Earth Atmosphere
52. 52
SOLO
7. Forces Acting on the Vehicle (continue – 5)
Gravitation Acceleration
Retaining only the first three terms of the
Gravitational Potential U (R, ) we obtain:ϕ
R
z
R
z
R
z
R
a
J
R
z
R
a
J
R
g
R
y
R
z
R
z
R
a
J
R
z
R
a
J
R
g
R
x
R
z
R
z
R
a
J
R
z
R
a
J
R
g
EEEE
z
EEEE
y
EEEE
x
E
E
E
⋅
+⋅−⋅
⋅−
−⋅
⋅−⋅−=
⋅
+⋅−⋅
⋅−
−⋅
⋅−⋅−=
⋅
+⋅−⋅
⋅−
−⋅
⋅−⋅−=
34263
8
5
15
2
3
1
34263
8
5
15
2
3
1
34263
8
5
15
2
3
1
2
2
4
44
42
22
22
2
2
4
44
42
22
22
2
2
4
44
42
22
22
µ
µ
µ
φ
φλ
φλ
sin
cossin
coscos
=
⋅=
⋅=
R
z
R
y
R
x
E
E
E
( ) 2/1222
EEE zyxR ++=
Air Vehicle in Ellipsoidal Earth Atmosphere
53. 53
SOLO
23. Local Level Local North (LLLN) Computations for an Ellipsoidal Earth Model
( )
( )
( )
( )
( )2
22
10
2
0
2
0
2
0
5
2
1
2
0
6
0
sin
sin1
sin321
sin1
sec/10292116557.7
sec/051646.0
sec/780333.9
26.298/.1
10378135.6
Ae
e
p
m
e
HR
RLatgg
g
LatfRR
LatffRR
LatfRR
rad
mg
mg
f
mR
+
+
=
+=
+−=
−=
⋅=Ω
=
=
=
⋅=
−
Lat
HR
V
HR
V
HR
V
Ap
East
Down
Am
North
East
Ap
East
North
tan
+
−=
+
−=
+
=
ρ
ρ
ρ
Lat
Lat
Down
East
North
sin
0
cos
Ω−=Ω
=Ω
Ω=Ω
DownDownDown
EastEast
NorthNorthNorth
Ω+=
=
Ω+=
ρφ
ρφ
ρφ
East
North
Lat
Lat
Long
ρ
ρ
−=
=
•
•
cos
( )
( ) ∫
∫
•
•
+=
+=
t
t
dtLatLattLat
dtLongLongtLong
0
0
0
0
SIMULATION EQUATIONS
Return to Table of Content
Air Vehicle in Ellipsoidal Earth Atmosphere
54. SOLO
54
References
Return to Table of Content
R.,H.,Battin, “Astronautical Guidance”, McGraw-Hill, 1964
George M. Siouris, “Aerospace Avionics System”, Academic Press, 1993, Appendix B
S. Hermelin, “Legendre Functions”
Broxmeyer, C,. “Inertial Navigation Systems”, McGraw-Hill, 1964
Averil B. Chatfield, “Fundamentals of High Accuracy Inertial Navigation”,
Progress in Astronautics and Aeronautics 174, 1997
X. Li, H-J. Götze, “Tutorial: Ellipsoid, Geoid, Gravity, Geodesy, and Geophysics”,
Geophysics, Vol. 66, No. 6, Nov-Dec. 2001
http://en.wikipedia.org/wiki/
Department of Defense, World Geodetic System 84, NIMA (National Imagery and
Mapping Agency) TR8350.2, Third Edition
http://earth-info.nga.mil/GandG/images/ww15mgh2.gif
http://earth-info.nga.mil/GandG/publications/tr8350.2/wgs84fin.pdf
Earth Gravitation
55. 55
SOLO
Technion
Israeli Institute of Technology
1964 – 1968 BSc EE
1968 – 1971 MSc EE
Israeli Air Force
1970 – 1974
RAFAEL
Israeli Armament Development Authority
1974 – 2013
Stanford University
1983 – 1986 PhD AA
56. 56
Vector AnalysisSOLO
Vector Operations in Various Coordinate Systems
Laplacian 2
∇=∇⋅∇
•Cartesian:
2
2
2
2
2
2
2
z
U
y
U
x
U
U
∂
∂
+
∂
∂
+
∂
∂
=∇
•Cylindrical:
2
2
2
2
22
2
2
2
2
2
2
2 1111
z
UUUU
z
UUU
U
∂
∂
+
∂
∂
+
∂
∂
+
∂
∂
=
∂
∂
+
∂
∂
+
∂
∂
∂
∂
=∇
θρρρρθρρ
ρ
ρρ
•Spherical:
( )
φθθ
θ
θθ
φθ 2
2
222
2
2
2
sin
1
sin
sin
11
,,
∂
∂
+
∂
∂
∂
∂
+
∂
∂
∂
∂
=∇
U
r
U
rr
U
r
rr
rU
57. 57
SOLO
Laplace Differential Equation in Spherical Coordinates
0
sin
1
sin
sin
11
2
2
222
2
2
2
=
∂
∂
+
∂
∂
∂
∂
+
∂
∂
∂
∂
=∇
φθθ
θ
θθ
U
r
U
rr
U
r
rr
U
Let solve this equation by the method of Separation of Variables,
by assuming a solution of the form :
( ) ( ) ( )φθφθ ,,, SrRrU =
Spherical Coordinates:
θ
ϕθ
ϕθ
cos
sinsin
cossin
rz
ry
rx
=
=
=
In Spherical Coordinates the Laplace equation becomes:
Substituting in the Laplace Equation and dividing by U gives:
0sinsin
sin
11
2
2
22
2
2
=
∂
∂
+
∂
∂
∂
∂
+
φθ
θ
θ
θ
θ
SS
Srrd
Rd
r
rd
d
Rr
The first term is a function of r only, and the second of angular
coordinates. For the sum to be zero each must be a constant, therefore:
λ
φθ
θ
θ
θ
θ
λ
−=
∂
∂
+
∂
∂
∂
∂
=
2
2
2
2
sinsin
sin
1
1
SS
S
rd
Rd
r
rd
d
R
58. 58
SOLO
Laplace Differential Equation in Spherical Coordinates
λ=
rd
Rd
r
rd
d
R
21
( ) ( )ϕθ,SrR=Φ
We get:
022
2
2
=−+ R
rd
Rd
r
rd
Rd
r λor:
Assume a solution of the form: R = C rα
, where α is a constant to be defined
and C is determined by the boundary conditions. Substituting in the Differential
Equation gives
( )[ ] 021 =−−− α
λααα rC
or:
( ) 01 =−+ λαα
Let define l as l (l+1):=λ
( ) ( ) ( ) 0111 2
=+−+=+−+ llll αααα
( ) ( )
−−
=
+±−
=
++±−
=
12
121
2
1411
2,1
l
llll
α
( )
=
+1
1
l
l
r
r
rR
59. 59
SOLO
( )1sinsin
sin
1
2
2
2
+−=
∂
∂
+
∂
∂
∂
∂
ll
SS
S φθ
θ
θ
θ
θ
( ) ( )ϕθ,SrR=Φ
We obtain:
Multiply this by S sin2
θ and put to get:( ) ( ) ( )φθφθ ΦΘ=,S
0
1
sinsinsin
1
2
2
2
=
Φ
Φ
+
+
Θ
∂
∂
Θ φ
θλ
θ
θ
θ
θ
d
d
d
d
Again, the first term, in the square bracket, and the last term must
be equal and opposite constants, which we write m2
, -m2
. Thus:
( )
Φ−=
Φ
=Θ
−++
Θ
∂
∂
2
2
2
2
2
0
sin
1sin
sin
1
m
d
d
m
ll
d
d
φ
θθ
θ
θθ
The Φ ( ) must be periodical in (a period of 2 π) and becauseϕ ϕ
this we choose the constant m2
, with m an integer. Thus:
( ) φφφ mbma sincos +=Φ
Laplace Differential Equation in Spherical Coordinates
( ) φφ
φ mjmj
ee +−
=Φ ,or
With m integer, we have the Orthogonality Condition
21
21
,
2
0
2 mm
mjmj
dee δπϕ
π
φφ
=⋅∫
+−
60. 60
SOLO
( ) ( ) ( ) ( )φθφθ ΦΘ= rRrU ,,
We get:
or:
( ) Θ+−=Θ−
Θ
+
Θ
1
sin
cot 2
2
2
2
ll
m
d
d
d
d
θθ
θ
θ
( ) 0
sin
1sin
sin
1
2
2
=Θ
−++
Θ
∂
∂
θθ
θ
θθ
m
ll
d
d
Laplace Differential Equation in Spherical Coordinates
Change of variables: t = cos θ
θθ dtd sin−=
td
d
d
d Θ
−=
Θ
θ
θ
sin
( ) td
d
t
td
d
t
td
d
d
d
td
d
td
d
td
d
td
d
d
d
d
d
d
d Θ
−
Θ
−=
Θ
+
Θ
=
Θ
−−=
Θ
=
Θ
−
2
2
2
cossin/1
2
2
2
2
2
1
sin
sinsinsinsin
θθ
θ
θθ
θθθθ
θθθ
( ) ( ) Θ
−
−++
Θ
−
Θ
−
Θ
=Θ
−++
Θ
+
Θ
=
=
2
2
2
2cos
2
2
2
2
1
1
sin
1cot0
t
m
ll
td
d
t
td
d
t
td
dm
ll
d
d
d
d t θ
θθ
θ
θ
We obtain:
( )
1cos
,2,1,00
1
12 2
2
2
2
≤⇒=
==Θ
−
−++
Θ
−
Θ
tt
m
t
m
ll
td
d
t
td
d
θ
Associate Legendre Differential Equation
61. 61
SOLO
( ) ( ) ( ) ( )φθφθ ΦΘ= rRrU ,,
Laplace Differential Equation in Spherical Coordinates
We obtain:
( )
1cos
,2,1,00
1
12 2
2
2
2
≤⇒=
==Θ
−
−++
Θ
−
Θ
tt
m
t
m
ll
td
d
t
td
d
θ
Associate Legendre Differential Equation
Let start with m = 0 with:
( )
1cos
0122
2
≤⇒=
=Θ++
Θ
−
Θ
tt
ll
td
d
t
td
d
θ
Legendre Differential Equation
They are named after Adrien-Marie Legendre. This
ordinary differential equation is frequently encountered in
physics and other technical fields. In particular, it occurs
when solving Laplace's equation (and related partial
differential equations) in spherical coordinates.
The Legendre polynomials were first introduced in 1785 by Adrien-Marie
Legendre, in “Recherches sur l’attraction des sphéroides homogènes”, as the
coefficients in the expansion of the Newtonian potential
Adrien-Marie Legendre
(1752 –1833(
62. SOLO
62
Legendre Polynomials
Olinde Rodrigues
(1794-1851)
Start from the function: ( ) .12
constktky
n
=−=
( ) 12
12:'
−
−==
n
ttkn
td
yd
y
( ) ( ) ( ) 22212
2
2
11412:''
−−
−−+−==
nn
ttnkntkn
td
yd
y
Let compute:
( ) ( ) ( ) ( ) ( ) '12211412''1
12222
ytntnttnkntknyt
nn
−+=−−+−=−
−
or: ( ) ( ) 02'12''12
=−−+− ynytnyt
Let differentiate the last equation n times with respect to t:
( )[ ] ( ) ( ) ( ) ( )
( ) ( ) ''1''2''1
00''1
3
''1
2
''1
1
''1''1
2
2
1
1
2
3
3
0
2
3
3
2
2
2
2
2
1
1
222
y
td
d
nny
td
d
tny
td
d
t
y
td
d
t
td
dn
y
td
d
t
td
dn
y
td
d
t
xd
dn
y
td
d
tyt
td
d
n
n
n
n
n
n
n
n
n
n
n
n
n
n
n
n
−
−
−
−
−
−
−
−
−
−
−++−=
+−
+−
+−
+−=−
( ) ( ) ( ) ( )
+−=
+−=− −
−
−
−
''12'
1
'12'12 1
1
1
1
y
td
d
ny
td
d
tny
td
d
t
td
dn
y
td
d
tnyt
td
d
n n
n
n
n
n
n
n
n
n
n
Derivation of Legendre Polynomials via Rodrigues’ Formula
Laplace Differential Equation in Spherical Coordinates
63. SOLO
63
Legendre Polynomials
Olinde Rodrigues
(1794-1851)
Start from the function: ( ) .12
constktky
n
=−=
( ) ( ) 02'12''12
=−−+− ynytnytDifferentiate n times with
respect to t:
( ) ( ) ''1''2''1 2
2
1
1
2
y
td
d
nny
td
d
tny
td
d
t n
n
n
n
n
n
−
−
−
−
−++−
( ) 02''12 1
1
=−
+−+ −
−
y
td
d
ny
td
d
ny
td
d
tn n
n
n
n
n
n
Define: a Polynomial( ) ( )[ ]n
n
n
n
n
t
td
d
k
td
yd
tw 1: 2
−==
( ) ( ) ( )[ ] 02'121'2''12
=−+−+−++− wnwnwtnwnnwtnwt
( ) ( ) ( ) ( )[ ] 02121'2''12
=−−+−+−++− wnnnnnwtnttnwt
( ) ( ) 01'2''12
=+−+− wnnwtwt
This is Legendre’s Differential Equation. We proved that one of the solutions
are Polynomials. We can rewrite this equation in a Sturm-Liouville Form:
( ) ( ) 0112
=+−
− wnnw
td
d
t
td
d
Derivation of Legendre Polynomials via Rodrigues’ Formula
Laplace Differential Equation in Spherical Coordinates
64. SOLO
64
Legendre Polynomials
Olinde Rodrigues
(1794-1851)
Let find k such that:
by choosing Pn (1) = 1
( ) ( )[ ]n
n
n
n
n
n t
td
d
k
td
yd
tP 12
−==
( ) ( )[ ] ( ) ( ) ( ) ( )
−+=
+−=−= ∑>0
22
1!2111
i
inn
v
n
u
n
n
n
n
n
n
n ttatnktt
td
d
ktk
td
d
tP
!2
1
n
k n
=
We obtain the Rodrigues Formula:
( ) ( )[ ]n
n
n
nn t
td
d
n
tP 1
!2
1 2
−=
Let use Leibnitz’s Rule (Binomial Expansion for the n Derivative
of a Product - with u:=(t-1)n
and v:=(t+1)n
):
( )
( )
( ) udvudvdnvddu
nn
vddunvdu
vdud
mnm
n
vud
nnnnn
n
m
mnmn
+++
−
++=
−
=⋅
−−−
=
−
∑
1221
0
!2
1
!!
!
We have:
( )
( )
1!2
!2
1
1
1!20
12
0
21
00
==
+++
−
++==
=
−−−
nkudvudvdnvddu
nn
vddunvdukxP n
xn
nnnnn
n
n
We can see from this Formula that Pn (t) is indeed a Polynomial of Order n in t.
Derivation of Legendre Polynomials via Rodrigues’ Formula
Laplace Differential Equation in Spherical Coordinates
65. SOLO
65
Legendre Polynomials
The first few Legendre polynomials are:
( )
( )
( )
( )
( )
( )
( )
( )
( )
( ) 256/63346530030900901093954618910
128/31546201801825740121559
128/35126069301201264358
16/353156934297
16/51053152316
8/1570635
8/330354
2/353
2/132
1
10
246810
3579
2468
357
246
35
24
3
2
−+++−
+−+−
+−+−
−+−
−+−
+−
+−
−
−
xxxxx
xxxxx
xxxx
xxxx
xxx
xxx
xx
xx
x
x
xPn n
Laplace Differential Equation in Spherical Coordinates
66. 66
SOLO
Orthogonality of Legendre Polynomials
Define ( ) ( )tPwtPv nm == :&:
We use Legendre’s Differential Equations:
( ) ( ) 011 2
=++
− vmm
td
vd
t
td
d
( ) ( ) 011 2
=++
− wnn
td
wd
t
td
d
Multiply first equation by w and integrate from t = -1 to t = +1.
( ) ( ) 011
1
1
1
1
2
=++
− ∫∫
+
−
+
−
dtwvmmdtw
td
vd
t
td
d
Integrate the first integral by parts we get
( ) ( ) ( ) 0111
1
1
1
1
2
0
1
1
2
=++−−− ∫∫
+
−
+
−
+=
−=
dtwvmmdt
td
wd
td
vd
tw
td
vd
t
t
t
In the same way, multiply second equation by v and integrate from t = -1 to t = +1.
( ) ( ) 011
1
1
1
1
2
=++−− ∫∫
+
−
+
−
dtwvnndt
td
wd
td
vd
t
Legendre Polynomials
67. 67
SOLO
Orthogonality of Legendre Polynomials
( ) ( ) 011
1
1
1
1
2
=++−− ∫∫
+
−
+
−
dtwvmmdt
td
wd
td
vd
t
Subtracting those two equations we obtain
( ) ( ) 011
1
1
1
1
2
=++−− ∫∫
+
−
+
−
dtwvnndt
td
wd
td
vd
t
( ) ( )[ ] ( ) ( )[ ] ( ) ( ) 01111
1
1
1
1
=+−+=+−+ ∫∫
+
−
+
−
dttPtPnnmmdtwvnnmm nm
This gives the Orthogonality Condition for m ≠ n
( ) ( ) nmdttPtP nm ≠=∫
+
−
0
1
1
To find let square the relation and integrate
between t = -1 to t = +1. Due to orthogonality only the integrals of terms
having Pn
2
(t) survive on the right-hand side. So we get
( )∫
+
−
1
1
2
dttPn
( )∑
∞
=
=
+− 0
2
21
1
n
n
n
tPu
utu
( )∑ ∫∫
∞
=
+
−
+
−
=
+− 0
1
1
22
1
1 2
21
1
n
n
n
dttPudt
utu
Legendre Polynomials
68. 68
SOLO
Orthogonality of Legendre Polynomials
( )∑ ∫∫
∞
=
+
−
+
−
=
+− 0
1
1
22
1
1 2
21
1
n
n
n
dttPudt
utu
( ) ( )
( )
1
1
1
ln
1
1
1
ln
2
1
21ln
2
1
21
1
2
21
1
2
1
1 2
<
−
+
=
+
−
−
=−+
−
=
−+
+=
−=
+
−∫ u
u
u
uu
u
u
tuu
u
dt
tuu
t
t
( ) ( ) ( ) ( ) ( ) ( ) ( )
∑∑∑
∞ ++∞ +∞ +
+
−−
−=
+
−
−−
+
−=−−+
0
11
0
1
0
1
1
1
1
1
1
1
1
1
1
1ln
1
1ln
1
n
uu
un
u
un
u
u
u
u
u
u
nn
n
n
n
n
n
( ) ( ) ( )
( )
( ) ( )
( ) ∑∑∑∑
∞∞ +∞ ++
+
∞ ++
+
=
+
=
+
−−
−+
+
−−
−=
0
2
0
12
0
0
1212
12
0
1212
2
12
2
12
1
2
12
1
1
12
1
1 n
nnn
n
nn
n
u
nn
u
un
uu
un
uu
u
Let compute first
Therefore
( )∑ ∫∑∫
∞ +
−
∞+
−
=
+
=
+− 0
1
1
22
0
2
1
1 2
12
2
21
1
dttPuu
n
dt
utu
n
nn
Comparing the coefficients of u2n
we get ( )
12
21
1
2
+
=∫
+
− n
dttPn
Legendre Polynomials
( ) ( ) nmmn
n
dttPtP δ
12
21
1 +
=∫
+
−
Hence
69. SOLO
69
Associated Legendre Functions
Let Differentiate this equation m times with respect to t, and use
Leibnitz Rule of
Product Differentiation: ( ) ( )[ ]
( )
( ) ( )
im
im
i
im
i
m
m
td
tgd
td
tsd
imi
m
tgts
td
d
−
−
=
∑ −
=⋅
0 !!
!
Start with
Legendre
Differential
Equation:
( ) ( ) ( ) ( ) 1011 2
≤=++
− ttwnntw
td
d
t
td
d
nn
or:
( ) ( ) ( ) ( ) ( ) 10121 2
2
2
≤=++−− ttwnntw
td
d
ttw
td
d
t nnn
( ) ( ) ( ) ( )
( ) ( )
( ) ( ) ( )
( )twmmtwtmtwttw
td
d
t
td
d m
n
m
n
m
nnm
m
1211
122
2
2
2
−−−−=
−
++
( ) ( )
( ) ( )
( )twmtwttw
td
d
t
td
d m
n
m
nnm
m
+=
+1
( ) ( )
( ) ( )
( ) ( ) ( )
( ) ( )
( ) ( )
( ) ( ) ( )
( )twnntwmtwttwmmtwtmtwt
m
n
m
n
m
n
m
n
m
n
m
n 122121
1122
++−−−−−−
+++
( ) ( )
( ) ( ) ( )
( ) ( ) ( )[ ] ( )
( ) 011121
122
=+−+++−−=
++
twmmnntwtmtwt
m
n
m
n
m
n
Laplace Differential Equation in Spherical Coordinates
70. SOLO
70
Associated Legendre Functions
( ) ( )
( ) ( ) ( )
( ) ( ) ( )[ ] ( )
( ) 011121
122
=+−+++−−
++
twmmnntwtmtwt
m
n
m
n
m
n
Define: ( ) ( )
( )twty
m
n=:
( ) ( )
( ) ( ) ( )
( ) ( ) ( )[ ] ( ) 011121 122
=+−+++−− tymmnntytmtyt
Now define: ( ) ( ) ( )tyttu
m
22
1: −=
Let compute:
( ) ( ) ( )1221
22
11 ytyttm
td
ud mm
−+−−=
−
( ) ( ) ( ) ( )11
22222
111 ytyttm
td
ud
t
mm
+
−+−−=−
( ) ( ) ( ) ( ) ( )
( ) ( ) ( )
( ) ( )21
221221221
2222222
1121111 ytyttmyttmyttmytm
td
ud
t
td
d mmmmm
+−
−+−+−−−−+−−=
−
( ) ( ) ( )
( ) ( )
( ) ( )[ ]{ } ( ) ( ) y
t
tm
mnnmmtymmnnytmytt
mm
−
+−+−+−++−+++−−−= 2
22
222
0
12222
1
11111211
We get:
( ) ( ) 0
1
11 2
2
2
=
−
−++
− u
t
m
nn
td
ud
t
td
d Associate Legendre
Differential Equation
Laplace Differential Equation in Spherical Coordinates
71. SOLO
71
Associated Legendre Functions
Define: ( ) ( ) ( )tw
td
d
ttu nm
mm
22
1: −=
We get: ( ) ( ) 0
1
11 2
2
2
=
−
−++
− u
t
m
nn
td
ud
t
td
d
Start with Legendre Differential Equation:
( ) ( ) ( ) ( ) 1011 2
≤=++
− ttwnntw
td
d
t
td
d
nn
Summarize
But this is the Differential Equation of Θ (θ) obtained by solving Laplace’s
Equation
by Separation of Variables in Spherical Coordinates .
02
=Φ∇
( ) ( ) ( ) ( )φθφθ ΦΘ=Φ rRr ,,
The Solutions Pn
m
(t) of this Differential Equation are called Associated Legendre
Functions, because they are derived from the Legendre Polynomials
( ) ( ) ( )tP
td
d
ttP nm
mm
m
n
22
1: −=
Laplace Differential Equation in Spherical Coordinates
72. SOLO
72
Associated Legendre Functions
Examples
( ) ( ) ( )tP
td
d
ttP nm
mm
m
n
22
1: −=
( ) ( ) 10 0
0
0 === tPtPn
( ) ( )
( )
( )
( ) ( )
( ) ( ) ( ) θ
θ
θ
θ
θ
θ
sin1
cos:
sin111
cos
2
1
21
1
1
1
cos
1
0
1
cos
2
1
22
1
21
1
1
−=−−=−=
===
=−=−==
=
−
=
=
t
t
t
tP
ttPtP
ttPtP
tt
td
d
ttPn
( ) ( ) ( )
( )
( )tP
mn
mn
tP
m
n
mm
n
!
!
1
+
−
−=
−
( ) ( )
( )
( )
( ) ( )
( )
( )
( ) ( )
( ) ( ) ( )
( )
( ) ( ) ( ) ( ) θ
θθ
θ
θθ
θ
θ
θ
θ
θ
θ
2
cos
22
2
22
2
cos
2
1
211
2
2cos2
2
0
2
cos
2
1
2
2
2
1
21
2
2
cos
2
2
2
2
2
2
22
2
sin
8
1
1
8
1
!4
!0
1
2
cossin
13
!3
1
1
2
1cos3
2
13
cossin313
2
13
1
sin313
2
13
12
1
2
2
1
=
−
=
−
=
=
=
=−=−=
−=−−=
−
=
−
==
=−=
−
−=
=−=
−
−==
t
t
tP
t
t
tP
t
tP
ttPtP
tttP
t
tPtP
tt
t
td
d
ttP
t
t
td
d
ttPn
( ) 10 =tP ( )
2
1
2
3 2
2 −= ttP( ) ttP =1
Laplace Differential Equation in Spherical Coordinates
73. SOLO
73
Associated Legendre Functions
Examples
( ) ( ) ( )tP
td
d
ttP nm
mm
m
n
22
1: −= ( ) ( ) ( )
( )
( )tP
mn
mn
tP
m
n
mm
n
!
!
1
+
−
−=
−
Laplace Differential Equation in Spherical Coordinates
74. SOLO
74
Associated Legendre Functions
Orthogonality of Associated Legendre Functions
( ) ( ) ( )[ ]n
mn
mnm
n
m
n t
td
d
t
n
tP 11
!2
1
: 222
−−= +
+
Let Compute
( ) ( ) ( ) ( )[ ] ( )[ ]∫∫
+
−
+
+
+
+
+
+
−
−−−=
1
1
222
1
1
111
!!2
1
dtt
td
d
t
td
d
t
qp
dttPtP
q
mq
mq
p
mp
mp
m
qp
m
q
m
p
Define X := x2
-1
( ) ( ) ( ) [ ] [ ]∫∫
+
−
+
+
+
+
+
+
−
−
=
1
1
1
1
!!2
1
dtX
td
d
X
td
d
X
qp
dttPtP q
mq
mq
p
mp
mp
m
qp
m
m
q
m
p
If p ≠ q, assume q > p and integrate by parts q + m times
[ ] [ ] mqidtX
td
d
vdX
td
d
X
td
d
u q
imq
imq
p
mp
mp
m
i
i
+==
= −+
−+
+
+
,,1,0
All the integrated parts will vanish at the boundaries t = ± 1 as long as there is a factor
X = x2
-1. We have, after integrating m + q times
( ) ( ) ( ) ( ) [ ]∫∫
+
−
+
+
+
+
+
++
−
−−
=
1
1
1
1
!!2
11
dtX
td
d
X
td
d
X
qp
dttPtP p
mp
mp
m
mq
mq
q
qp
mqm
m
q
m
p
75. SOLO
75
Associated Legendre Functions
( ) ( ) ( ) ( ) [ ] 1:
!!2
11 2
1
1
1
1
−=
−−
= ∫∫
+
−
+
+
+
+
+
++
−
xXdtX
td
d
X
td
d
X
qp
dttPtP p
mp
mp
m
mq
mq
q
qp
mqm
m
q
m
p
Because the term Xm
contains no power greater than x2m
, we must have
q + m – i ≤ 2 m
or the derivative will vanish. Similarly,
p + m + i ≤ 2 p
Adding both inequalities yields
q ≤ p
which contradicts the assumption that q > p, therefore is no solution for i and the
integral vanishes.
Let expand the integrand on the right-side using Leibniz’s formula
( )
( )∑
+
=
++
++
−+
−+
+
+
+
+
−+
+
=
mq
i
p
imp
imp
m
imq
imq
qp
mp
mp
m
mq
mq
q
X
td
d
X
td
d
imqi
mq
XX
td
d
X
td
d
X
0 !!
!
( ) ( ) qpdttPtP m
q
m
p ≠=∫
+
−
0
1
1
This proves that the Associated Legendre Functions are Orthogonal (for the same m).
Orthogonality of Associated Legendre Functions
76. SOLO
76
Associated Legendre Functions
( )[ ] ( ) ( ) 1:
!!2
11 2
1
1
2
21
1
2
−=
−−
= ∫∫
+
−
+
+
+
++
−
xXdtX
td
d
X
td
d
X
pp
dttP p
mp
mp
m
mp
mp
p
p
mp
m
p
Let expand the integrand on the right-side using Leibniz’s formula
( )
( )∑
+
=
++
++
−+
−+
+
+
+
+
−+
+
=
mp
i
p
imp
imp
m
imp
imp
pp
mp
mp
m
mp
mp
p
X
td
d
X
td
d
impi
mp
XX
td
d
X
td
d
X
0 !!
!
For the case p = q we have
Because X = x2
– 1 the only non-zero term is for i = p - m
( )[ ] ( ) ( )
( ) ( ) ( )
( ) ( )
1:
!2!!2
!1 2
1
1
!2
2
2
!2
2
2
22
1
1
2
−=⋅
−
+−
= ∫∫
+
−
+
−
xXdtX
td
d
X
td
d
X
mmpp
mp
dttP
p
p
p
p
m
m
m
m
p
p
p
m
p
( ) ( ) ( )
( ) ( )
( ) ( ) ( ) ( )
( ) ( )
( )
( ) ( )
( )
( )
( )!
!
12
2
sin1
!!2
!2!1
1
!!2
!2!1
!12
!2
1
0
12
22
cos1
1
2
22
212
mp
mp
p
d
mpp
pmp
dtx
mpp
pmp
p
p
pp
p
ptp
X
p
p
p
p
−
+
⋅
+
=
−
−
+−
=−
−
+−
=
+
−
+
=+
−
+
∫∫
θθ
πθ
Orthogonality of Associated Legendre Functions
77. SOLO
77
Associated Legendre Functions
( ) ( ) ( ) ( ) ( )
( ) qp
m
q
m
p
t
m
q
m
p
mp
mp
p
dPPdttPtP ,
0
cos1
1
!
!
12
2
sincoscos δθθθθ
πθ
−
+
+
== ∫∫
=+
−
Therefore the Orthonormal Associated Legendre Functions is
( ) ( )
( )
( ) mnmP
mn
mnn
Θ
m
n
m
n ≤≤−
+
−+
= θθ cos
!
!
2
12
cos
Orthogonality of Associated Legendre Functions
78. 78
SOLO
Absolute Angular Momentum Relative to a
Reference Point O
The Absolute Momentum Relative to a Reference
Point O, of the particle of mass dmi at time t is
defined as:
( ) ( ) iiOiiiOiiOiO dmVrdmVRRPdRRHd
×=×−=×−= ,, :
The Absolute Momentum Relative to a Reference Point O, of the mass m (t) is defined
as:
( ) ( ) ∑∑∑ ===
×=×−=×−=
N
i
i
I
i
Oi
N
i
iiOi
N
i
iOiO dm
td
Rd
rdmVRRPdRRH
1
,
11
, :
By taking a very large number N of particles, we go from discrete to continuous ∫⇒∑
∞→
=
NN
i 1
( )( )
( )( ) ( )
∫ ×=∫ ×−=∫ ×−=
tm
O
tm
O
tv
OO dmVrdmVRRdvVRRH
,, ρ
The Absolute Momentum Relative to a Reference Point O, of the system (including the
mass entering (+)/leaving (-) through surface S), at time t + Δt is given by:
( ) ( )∑∑ ∆
∆+×∆++
∆+×∆+=∆+
= openings
iflow
I
iflow
I
iflow
OiflowOiflow
N
i
i
I
i
I
i
OiOiOO m
td
Rd
td
Rd
rrdm
td
Rd
td
Rd
rrHH
,,
1
,,,,
EQUATIONS OF MOTION OF A VARIABLE MASS SYSTEM
SIMPLIFIED PARTICLE APPROACH
79. 79
SOLO
Absolute Angular Momentum Relative to a
Reference Point O (continue – 1)
By subtracting
I
O
t
I
O
t
H
td
Hd
∆
∆
=
→∆
,
0
,
lim
( ) ( )
t
dm
td
Rd
rm
td
Rd
td
Rd
rrdm
td
Rd
td
Rd
rr
openings
N
i
i
I
i
iOiflow
I
iflow
I
iflow
OiflowOiflow
N
i
i
I
i
I
i
OiOi
t ∆
×−∆
∆+×∆++
∆+×∆+
=
∑ ∑∑ ==
→∆
1
,,
1
,,
0
lim
∑∑∑ ×+×+×=
== openings
iflow
I
iflow
Oiflow
N
i
i
I
iOi
N
i
i
I
i
Oi m
td
Rd
rdm
td
Rd
td
rd
dm
td
Rd
r
,
1
,
1
2
2
,
Now let add the constraint that at time t the flow at the opening is such
that
iopenS
( ) ( ) ( ) ( )trtrtRtR OiflowOiopeniflowiopen ,,
=→=
to obtain (next page)
EQUATIONS OF MOTION OF A VARIABLE MASS SYSTEM
SIMPLIFIED PARTICLE APPROACH
( )( )
( )( ) ( )
∫ ×=∫ ×−=∫ ×−=
tm
O
tm
O
tv
OO dmVrdmVRRdvVRRH
,, ρ
dividing by Δt, and taking the limit, we get
from ( ) ( )∑∑ ∆
∆+×∆++
∆+×∆+=∆+
= openings
iflow
I
iflow
I
iflow
OiflowOiflow
N
i
i
I
i
I
i
OiOiOO m
td
Rd
td
Rd
rrdm
td
Rd
td
Rd
rrHH
,,
1
,,,,
80. 80
SOLO
Absolute Angular Momentum Relative to a
Reference Point O (continue – 2)
∑∑∑ ×+×+×=
== openings
iflow
I
iflow
Oiopen
N
i
i
I
i
I
Oi
N
i
i
I
i
Oi
I
O
m
td
Rd
rdm
td
Rd
td
rd
dm
td
Rd
r
td
Hd
,
1
,
1
2
2
,
,
( )∑ ×−+∑ ×
−+∑ ×=
== openings
iflow
I
iflow
Oiopen
N
i
i
I
i
I
O
I
i
N
i
i
I
i
Oi m
td
Rd
RRdm
td
Rd
td
Rd
td
Rd
dm
td
Rd
r
11
2
2
,
( )∑ ×−+∑×−∑ ×=
== openings
iflow
I
iflow
Oiopen
N
i
i
I
i
I
O
N
i
i
I
i
Oi m
td
Rd
RRdm
td
Rd
td
Rd
dm
td
Rd
r
11
2
2
,
By taking a very large number N of particles, we go from discrete to continuous ∫⇒∑
∞→
=
NN
i 1
( )
( )∑ ×−+×−∫ ×=
openings
iflowiflowOiopenO
tm
I
O
I
O
mVRRPVdm
td
Rd
r
td
Hd
2
2
,
,
( ) ( ) ∑∑ −+=−−+=
openings
OiopeniflowO
I
O
openings
OiopeniflowO
I
O
rmVm
td
cd
RRmVm
td
cd
tP ,
,,
Substitute to obtain
( )
( ) ( )∑ ×−+×
∑ −−++∫ ×=
openings
iflowiflowOiopenO
openings
iflowOiopenO
I
O
tm
I
O
I
O
mVRRVmRRVm
td
cd
dm
td
Rd
r
td
Hd
,
2
2
,
,
or
( )
( )∑ −×+×+∫ ×=
openings
iflowOiflowOiopenO
I
O
tm
I
O
I
O
mVVrV
td
cd
dm
td
Rd
r
td
Hd
,
,
2
2
,
,
EQUATIONS OF MOTION OF A VARIABLE MASS SYSTEM
SIMPLIFIED PARTICLE APPROACH
81. 81
SOLO
Absolute Angular Momentum Relative to a
Reference Point O (continue – 3)
We obtained
( )( )
( )( ) ( )
∫ ×=∫ ×−=∫ ×−=
tm
O
tm
O
tv
OO dmVrdmVRRdvVRRH
,, ρ
Substitute in the previous equation
OIO
O
O
O
I
O
I
O
I
OO r
td
rd
V
td
rd
td
Rd
td
Rd
VrRR ,
,,
, :&
×++=+==+= ←ω
( )( ) ( )
∫
×++×=∫ ×−= ←
tm
OIO
O
O
OO
tm
OO dmr
td
rd
VrdmVRRH ,
,
,,
ω
( )
( )
( ) ( )
∫
×+∫ ××+×
∫= ←
tm
O
O
O
tm
OIOOO
tm
O dm
td
rd
rdmrrVdmr ,
,,,,
ω
We obtain
(a) (b) (c)
Let develop those three expressions (a), (b) and (c).
where is the angular velocity vector from I to O.IO←ω
EQUATIONS OF MOTION OF A VARIABLE MASS SYSTEM
SIMPLIFIED PARTICLE APPROACH
82. 82
SOLO
Absolute Angular Momentum Relative to a
Reference Point O (continue – 4)
(a)
( ) ( ) ( ) ( ) ( )
( ) OOC
tm
OC
tm
OC
tm
OC
tm
C
tm
O cmRRdmrdmrdmrdmrdmr ,,,,,,
=−===+= ∫∫∫∫∫
Where we used because C is the Center of Mass (Centroid) of the system.
( )
0, =∫tm
C dmr
( )
OOOOCO
tm
O VcVrmVdmr
×=×=×
∫ ,,,
( )
( )
( )[ ]( )
IOOIO
tm
OOOO
tm
OIBO Idmrrrrdmrr ←←← ⋅=⋅∫ −⋅=∫ ×× ωωω
,,,,,,, 1(b)
where
( )[ ]
( )
∫ −⋅=
tm
OOOOO dmrrrrI ,,,,, 1:
2nd
Moment of Inertia Dyadic of all the
mass m(t) relative to O
We obtain (a) + (b) + (c)
( )( ) ( )
( )
( ) ( )
∫
×+∫ ××+×
∫=∫ ×−= ←
tm
O
O
O
tm
OIOOO
tm
O
tv
OO dm
td
rd
rdmrrVdmrvdVRRH ,
,,,,, :
ωρ
( )
∫
×+⋅+×= ←
tm
O
O
OIOOOO dm
td
rd
rIVc ,
,,,
ω
EQUATIONS OF MOTION OF A VARIABLE MASS SYSTEM
SIMPLIFIED PARTICLE APPROACH
83. SOLO
Absolute Angular Momentum Relative to a
Reference Point O (continue – 4)
( )[ ]
( )
∫ −⋅=
tm
OOOOO dmrrrrI ,,,,, 1:
2nd
Moment of Inertia Dyadic of all the
mass m(t) relative to O
EQUATIONS OF MOTION OF A VARIABLE MASS SYSTEM
SIMPLIFIED PARTICLE APPROACH
=
O
O
O
O
z
y
x
r
,
,
,
,
( )[ ] [ ] [ ]OOO
O
O
O
O
O
O
OOOOOOO zyx
z
y
x
z
y
x
zyxrrrr ,,,
,
,
,
,
,
,
,,,,,,,
100
010
001
1
−
=−⋅
( )
∫
+−−
−+−
−−+
=
tm
OOOOOO
OOOOOO
OOOOOO
O dm
yxzyzx
zyzxyx
zxyxzy
I
2
,
2
,,,,,
,,
2
,
2
,,,
,,,,
2
,
2
,
, :
Averil B. Chatfield, “Fundamentals of High Accuracy Inertial Navigation”, Progress in Astronautics and Aeronautics 174, 1997
George M. Siouris, “Aerospace Avionics System”, Academic Press, 1993, Appendix B
R.,H.,Battin, “Astronautical Guidance”, McGraw-Hill, 1964
S. Hermelin, “Legendre Functions”
R.,H.,Battin, “Astronautical Guidance”, McGraw-Hill, 1964
S. Hermelin, “Legendre Functions”
R.,H.,Battin, “Astronautical Guidance”, McGraw-Hill, 1964
S. Hermelin, “Legendre Functions”
R.,H.,Battin, “Astronautical Guidance”, McGraw-Hill, 1964
S. Hermelin, “Legendre Functions”
Averil B. Chatfield, “Fundamentals of High Accuracy Inertial Navigation”, Progress in Astronautics and Aeronautics 174, 1997
George M. Siouris, “Aerospace Avionics System”, Academic Press, 1993, Appendix B
Averil B. Chatfield, “Fundamentals of High Accuracy Inertial Navigation”, Progress in Astronautics and Aeronautics 174, 1997
George M. Siouris, “Aerospace Avionics System”, Academic Press, 1993, Appendix B
http://en.wikipedia.org/wiki/World_Geodetic_System
Averil B. Chatfield, “Fundamentals of High Accuracy Inertial Navigation”, Progress in Astronautics and Aeronautics 174, 1997
http://earth-info.nga.mil/GandG/images/ww15mgh2.gif
http://earth-info.nga.mil/GandG/publications/tr8350.2/wgs84fin.pdf
Department of Defense, World Geodetic System 84, NIMA (National Imagery and Mapping Agency) TR8350.2, Third Edition
George M. Siouris, “Aerospace Avionics System”, Academic Press, 1993, Appendix B
http://en.wikipedia.org/wiki/Latitude
Averil B. Chatfield, “Fundamentals of High Accuracy Inertial Navigation”, Progress in Astronautics and Aeronautics 174, 1997
George M. Siouris, “Aerospace Avionics System”, Academic Press, 1993, Appendix B
Averil B. Chatfield, “Fundamentals of High Accuracy Inertial Navigation”, Progress in Astronautics and Aeronautics 174, 1997
George M. Siouris, “Aerospace Avionics System”, Academic Press, 1993, Appendix B
Wallace, P.R., “Mathematical Analysis of PhysicaL Problems”, Dover 1972, 1984
Wallace, P.R., “Mathematical Analysis of PhysicaL Problems”, Dover 1972, 1984
Wallace, P.R., “Mathematical Analysis of PhysicaL Problems”, Dover 1972, 1984
Wallace, P.R., “Mathematical Analysis of PhysicaL Problems”, Dover 1972, 1984
Wallace, P.R., “Mathematical Analysis of PhysicaL Problems”, Dover 1972, 1984