The Four-Vectors (4-Vectors) and Lorentz Invariants of Special Relativistic (SR) theory are fundamental entities that accurately, precisely, and beautifully describe the physical properties of the world around us. While it is known that SR is not the "deepest" theory, it is valid for the majority of the known universe. It is believed to apply to all forms of interaction, including that of fundamental particles and quantum effects, with the only exception being that of large-scale gravitational phenomena, where spacetime itself is significantly curved, for which General Relativity (GR) is required. The SR 4-vector notation is one of the most powerful tools in understanding the physics of the universe, as it simplifies a great many of the physical relations.
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A vector is a mathematical object which has both magnitude and
direction. It is a powerful tool for describing physical phenomena. A common 3-vector is the velocity vector (vx, vy,
vz), which tells you
in what direction and how fast something is moving. One might use the (x, y, z) coordinates to
write down the velocity vector of some object in the laboratory. That
would be an example of a rectilinear coordinate system. Another
person might use a coordinate system that is rotated wrt. the first
observer, with components (y', x', z). The same vector might also be
described by the (r, θ, φ) spherical coordinate system.
Within a given coordinate system, each component is typically
orthogonal to each other component. While these different coordinate
systems will usually have different numbers in the vector 3-tuple,
they nevertheless describe the same vector and the same physics.
Hence, the vector can be considered the "primary" element,
which is then described by any number of different coordinate
systems, which simply represent one point-of-view of the given
vector.
The extension of 3-vectors to that of 4-vectors is a
simple idea. Let's imagine some event in spacetime. The location of the
event in the Newtonian world would be it's 3-position (x,y,z), and
the time (t) at which it occurs. In the Newtonian world these are
totally separate ideas. SR unites them into a single object. The
location of the event in the SR world would be it's 4-position
(ct,x,y,z). All that we have done is to insert the time (t) into the
vector as another component. The factor of (c) is put with it to make
the dimensional units work out right. ( [m/s]*[s] = [m]). So, each
component now has overall units of [m] for this 4-vector. This rather
simple idea, combined with the postulates of SR, lead to some amazing
results and elegant simplifications of physical concepts...
There
are two postulates which lead to all of SR-Special Relativity:
(1)
The laws of physics are the same for all inertial reference frames.
This means the form of the physical laws should not change for
different inertial observers. This can be also restated as "All
inertial observers measure the same interval magnitude between two
events". I say it this way because all of experimental physics
ultimately boils down to taking a measurement.
(2) The speed of
light (c) in vacu is the same for all inertial reference frames.
This is the result of millions of independent measurements, all
confirming the same observation. This differentiates SR from Galilean
invariance, which also obeys the first postulate.
4-vectors
are tensorial entities which display Poincare' Invariance, meaning
they leave invariant the differential squared interval (ds)2
= (cdt)2-dx2-dy2-dz2. A
consequence of this invariant measurement is that any physical
equation which is written in Poincare' Invariant form is
automatically valid for any inertial reference frame, regardless of
how coordinate systems are arranged. Transformations which leave
these vectors unchanged include fixed translations through space
and/or time, rotations through space, and boosts (coordinate systems
moving with constant velocity) through spacetime. Since 4-vectors are
tensors, and Poincare' Invariant, they can be used to describe and
explain the physical properties that are observed in nature. Although
the vector components may change from one reference frame to another,
the 4-vector itself is an invariant, meaning that it gives valid
physical information for all inertial observers. Likewise, the scalar
products of Lorentz Invariant 4-vectors are themselves invariant
quantities, known as Lorentz Scalars. Lorentz Invariance is a special
subset of Poincare' Invariance.
The reason that I really like
this notation is that it beautifully and elegantly displays the
relations between lots of different physical properties. It also
devolves very nicely into the limiting/approximate Newtonian cases of
v<<c by letting γ -->1 and dγ/dt -->0. SR
tells us that several different physical properties are actually dual
aspects of the same thing, with the only real difference being one's
point of view, or reference frame. Examples include: (Time , Space),
(Energy , Momentum), (Power , Force), (Frequency , WaveNumber),
(ChargeDensity , CurrentDensity), (EM-Potential ,
EM-VectorPotential), (Time Differential, Spatial Gradient), etc. Also, things
are even more related than that. The 4-Momentum is just a constant
times 4-Velocity. The 4-WaveVector is just a constant times
4-Momentum. In addition, the very important conservation/continuity
equations seem to just fall out of the notation. The universe
apparently has some simple laws which can be easy to write down by
using a little math and a super notation.
QM = Quantum Mechanics SR = Special Relativity
SM =
Statistical Mechanics GR = General Relativity
|
length/time |
[m] meter <*> [s] second |
Count of the quantity of separation or distance; Location of events in spacetime |
|
mass |
[kg] kilogram |
Count of the quantity of matter; (the "stuff" at an event) |
|
EMcharge |
[C] Coulomb |
Count of the quantity of electric charge; the Coulomb is more fundamental than the Ampere |
|
temperature |
[ŗK] Kelvin |
Count of the quantity of heat (statistical) |
Velocity
v or u: v = velocity, but u is historically used in SR notation
Minkowski Flat (Pseudo-Euclidian) Spacetime Metric:
ημν
= gμν = gμν =
Diag[+1,-1,-1,-1]
Dimensionless SR Factors:
β
= (v/c) = [0..1]: Relativistic Beta factor, the fraction of the speed of light c
β
= (u/c): Vector form of Beta factor, u is the velocity
γ[u] = dt/dτ:
Lorentz Gamma Scaling Factor (Relativistic Gamma factor)
γ = (1 / √[1-(v/c)2]
) = (1 / √[1-(u·u/c2)] ):
Lorentz Gamma Scaling Factor (~1 for v<<c), (>>1 for
v~c)
γ = (1 / √[1-β2] ) = (1 /
√[1-β·β] ): Lorentz Gamma
Scaling Factor (~1 for β<<1), (>>1 for β~1)
γ = (1 / √[1-β2] ) = 1/√[(1+|β|)/(1-|β|)]
φ
= Ln[γ(1+ β)] ~ Atanh[β]: BoostParameter/Rapidity (which remains
additive in SR, unlike v)
eφ =
γ(1+β) = √[(1+β)/(1-β)]
β =
Tanh[φ], γ = Cosh[φ], γβ = Sinh[φ], φ
= Rapidity (which remains strictly additive in SR, unlike v)
D = 1 / [γ(1 - β Cos[θ] )] = 1 / [γ(1 - β·n )]:
Relativistic Doppler Factor
Temporal Factors:
τ =
t / γ : Proper Time = Rest Time (time as measured in a frame at
rest)
dτ = dt / γ : Differential of Proper Time
d/dτ
= γ d/dt = U·∂ : Differential wrt Proper
Time
Useful SR Formulas:
V·V
= Vo·Vo : Invariant interval is often easier to
calculate in rest frame coordinates
√[1+x] ~ (1+x/2) for
x ~ 0 : Math relation often used to simplify Relativistic eqns.
to Newtonian eqns.
1/√[1+x] ~ (1-x/2) for
x ~ 0 : Math relation sometimes used to simplify Relativistic eqns.
to Newtonian eqns.
δuv = Delta function = (1 if u
= v, 0 if u ≠ v)
γ = (1 / √[1-(u·u/c2)]) = c/√[c2-v2]
= c/√[c2-u·u]
γ2
= c2/(c2-v2) = c2/(c2-u·u)
= 1/(1-
β2)
c2/γ2
= (c2-v2)
v
γ = c √[γ2-1]
β γ =
√[γ2-1]
(1-β2)γ2 = 1
β2γ2 = γ2-1
β2γ = (γ-1/γ)
c2 dγ = γ3
v dv
d(γ v) = c2 dγ / v = γ3 dv
dγ = γ3
v dv / c2 = γ3 β dβ
dβ
= dv / c
dγ/dv = γ3
v / c2
d(γ-1)/dv = - γ
v / c2
γ' = dγ/dt = (γ3 v
dv/dt)/c2 = (γ3 u·a)/c2
= ar·u/c2
γ''
= dγ'/dt = d2γ/dt2 =
(γ3/c2)*[(3γ2/c2)(u·a)2
+ (u'·a) + (u·a')]
u2 = u2
u·u'
= uu' = ua
(|u x a|)2 + (u·a)2 = u2a2
sin2 + cos2
= 1
**NOTE**
All
results below use the SR Minkowski Metric =
Diag[+1,-1,-1,-1].
If you wish to do GR, with other metrics, then
some results below may need GR modification, such as the GR √[-g]
for whichever metric you are using...
You have been warned.
There are several different SR notations available that are,
mathematically speaking, equivalent.
However, some are easier to
employ than others. I have used that one which seems the most
practical and least error-prone.
If you mix notations, you will get errors!
Always check notation conventions
in SR & 4-Vector references, they are all relative ;-)
Minkowski
SR Metric (time 0-component positive), for which ημν
= gμν = gμν = Diag[+1,-1,-1,-1] =
Diag[+1,-1]
Signature[ημν] = -2
A
= (at,ax,ay,az) = (a0,a1,a2,a3)
=
(a0,a)
time (a0) in the 0th coord. ( some alternate
notations use time as a4 )
Note that these are not exponents, they are upper tensor indices
Intervals:
Time/Temporal
(+ interval) = 0 coordinate ( some alternate notations use time
as - interval and space as the + interval)
Light/Null (0
interval)
Space/Spatial (- interval) = 1,2,3 coordinates
Temporal
Components: Future(+), Now(0), Past(-)
4-Vector Name: always
references the "Spatial" 3-vector component (basically
trying to extend the Newtonian 3-vector to SR 4-vector)
4-Vector
Magnitude: usually references the "temporal" scalar
component (because many vectors in the rest frame only have a
temporal component)
4-Vector Symbols: A = Aμ
= (a0,a) = (a0,a1+a2+a3)
= (a0,a1,a2,a3), where
the raised index indicates dimension, not exponent
4-Vector
c-Factor: always applied to "Temporal" scalar component, as
necessary to give consistent dimensional units for all vector
components (a0,a1,a2,a3)
<==> (ct,x,y,z) = (ct,x)
*Note* c-Factor can be on the top, as ( ct , x , y , z ) = [m], or on
bottom, as ( E/c , px , py , pz )
=
[kg m s-1]
*Note*
P = (E/c, p) = (mc, p); the 4-Momentum is a good
case showing top or bottom, with E = mc2
4-Vector Computer HTML
Representation:
SR 4-vector = {BOLD UPPERCASE}
= A
time scalar component = {regular lowercase}
= a0
space
3-vector component = {bold lowercase} = a
Contraction & Dilation
Relativistic
Component: v --> vo in a rest-frame, typically v = γ
vo (dilation) or v = (1/γ) vo
(contraction)
eg. t = γ to (time dilation), L =
(1/γ) Lo (length contraction)
Generally, time-like quantities get dilated, space-like quantities get
contracted by motion
Also, I typically denote "at-rest" invariant quantities with a
"naught", or "o", i.e.:
Lo (invariant rest length = proper length), relativistic
length L =
(1/γ) Lo
Vo (invariant rest volume), relativistic volume V =
(1/γ) Vo
mo (invariant rest mass), relativistic mass m = γ mo
Eo (invariant rest energy), relativistic energy E = γ Eo
ωo (invariant rest ang-frequency), relativistic
ang-frequency ω
= γ ωo
ρo (invariant rest charge-density), relativistic
charge-density ρ = γ ρo
no (invariant rest number-density), relativistic
number-density n = γ no
to (invariant rest time = proper time), relativistic
time t = γ
to = γ τ
etc.
This avoids the confusion of some texts which use just "m" as
invariant mass, or just "ρ" as invariant charge-density.
It also helps to avoid confusion such as:
If the mass m of an object
increases
with velocity, wouldn't it have be a black hole in some reference
frames (near
c), since the mass increases with velocity.
Answer - no. The rest mass mo does not change.
The
relativistic mass is simply an "apparent" mass, how the object is
velocity-related to an observer, not how much "stuff" is in it...
The apparent increase is fully due to the gamma factor( γ ), which is
simply
a reflection of relative motion.
Imaginary unit:
( i ) used only for QM phenomena, not for SR frame transformations or
metric. To follow up on a quote " ict was put to the sword
".
This allows all the purely SR stuff to use only real
numbers. Imaginary/complex stuff apparently only enters the
scene via QM.
( some alternate notations use the imaginary unit (
i ) in the components/frame transformations/metric )
So, in
summary, this notation allows:
easy recovery of Newtonian cases
by allowing (γ-->1, dγ-->0) when (v<<c)
easy separation of SR vs Newtonian
concepts, with the Newtonian 3-vector (a) extending naturally
into the SR 4-vector (A)
easy
separation of SR vs QM concepts, no ict's -- ( i ) only enters into
QM concepts, such as Photon Polarization, Quantum Probability Current,
etc.
easy separation of relativistic quantities vs. invariant quantities, E
= γ
Eo
reduction in number of
minus signs (-), eg. U·U = c2, P·P
= (moc)2: the square magnitudes of velocity,
momentum, and other velocity-based vectors are positive
The main assumption of SR, or GR for that matter, is that the structure of spacetime is described by a metric gμν. A metric tells how the spacetime is put together, or how distances are measured within the spacetime. These distances are known as intervals. In GR, the metric may take a number of different values, depending on various circumstances which determine its curvature. We are interested in the flat/pseudo-Euclidean spacetime of SR, also known as the Minkowski Metric, for which ημν = gμν = gμν = Diag[+1,-1,-1,-1].
|
"Flat" SpaceTime |
|
|
|
|
|
t |
1 |
0 |
0 |
0 |
|
x |
0 |
-1 |
0 |
0 |
|
y |
0 |
0 |
-1 |
0 |
|
z |
0 |
0 |
0 |
-1 |
gμα gμβ = δαβ =
(4 if α = β for Minkowski)
g = - Det[gμν]
= -1 (for Minkowski) not a scalar invariant
Sqrt[-g]ρ: Scalar
density
There are other ways of defining the metrics and
4-vectors available in SR which lead to the same results, but this
particular notation has some nice qualities which place it above the
others. First, it shows the difference between time and space in the
metric. We perceive time differently than space, despite there being
only spacetime. Also, this metric gives all of the SR relations
(frame transformations) without using the imaginary unit ( i ) in the
transforms. This is important, as ( i ) is absolutely essential for
the complex wave functions once we get to QM. It is not needed, and
would only complicate and confuse matters in SR. This metric will
allow us to separate the "real" SR stuff from the
"complex/imaginary" QM stuff easily. It also allows for the
possibility of complex components in SR 4-vectors. The choice
of +1 for the time component simplifies the derived equations later
on, as it allows rest frame square-magnitudes to be positive for most quantities
of interest.
ημν = gμν
= gμν = DiagnolMatrix[1,-1,-1,-1]: Minkowski
Spacetime Metric-the "flat" spacetime of SR
A
= Aμ = (at,ax,ay,az)
= (a0,a1,a2,a3) = (a0,a):
Typical SR 4-vector
Aμ
= (at,-ax,-ay,-az) =
(a0,-a1,-a2,-a3) =
(a0,-a): Typical SR 4-covector, we can always get
the 4-vector form with Aμ = gμνAμ
Basically, this has the effect of
putting a minus sign on the space component
B = Bμ
= (bt,bx,by,bz) =
(b0,b1,b2,b3) = (b0,b):
Another typical SR 4-vector
A·B = gμν
Aμ Bν = Aν Bν
= Aμ Bμ = +a0b0-a1b1-a2b2-a3b3
= (+a0b0-a·b): The Scalar
Product relation, used to make SR invariants
c(A + B)
= (cA + cB) scalar multiplication
A·A
= A2 = (+a02 - a12
- a22 - a32) = (+a02
- a·a) magnitude squared, which can be { - , 0 ,
+ }
A = |A| = √|A2| >= 0
absolute magnitude or length, which can be { 0 , + }
A·B
= B·A commutative, with the exception of the (∂)
operator, since it only acts to the right
A·(B
+ C) = A·B + A·C
distributive
d(A·B) = d(A)·B
+ A·d(B) differentiation
B = d(A)/dθ,
where θ is a Lorentz Scalar Invariant
Aproj
= (A·B)/(B·B) B
= Projection of A along B
A||
= (A·B)/(B·B) B
= Component of A parallel to B
A⊥
= A - A||
A⊥
=A - (A·B)/(B·B) B
= Component of A perpendicular to B
==========
if A·A
= const
then
dA1dA2dA3 / A0
dA0dA2dA3 / A1
dA0dA1dA3 / A2
dA0dA1dA2 / A3
are scalar invariants
from Jacobian derivation
============
if Aμ dXμ
= invariant for any dXμ, then Aμ is a
4-vector
ημν
Λμα Λνβ
= ηαβ
Λαμ Λμβ
= dαβ
A'μ = Λμν
Aν: Lorentz Transform (Transformation tensor which
gives relations between alternate boosted inertial reference
frames)
Λμ'ν
= (∂Xμ'/∂Xν)
Λμν = (for x-boost)
|
γ |
-(vx/c)γ |
0 |
0 |
|
-(vx/c)γ |
γ |
0 |
0 |
|
0 |
0 |
1 |
0 |
|
0 |
0 |
0 |
1 |
or
|
γ |
-βxγ |
0 |
0 |
|
-βxγ |
γ |
0 |
0 |
|
0 |
0 |
1 |
0 |
|
0 |
0 |
0 |
1 |
General Lorentz
Transformation
Λμν = (for
n-boost)
|
γ |
-βxγ |
-βyγ |
-βzγ |
|
-βxγ |
1+(γ-1)(βx/β)2 |
( γ-1)(βxβy/β)2 |
( γ-1)(βxβz/β)2 |
|
-βyγ |
( γ-1)(βyβx/β)2 |
1+( γ-1)(βy/β)2 |
( γ-1)(βyβz/β)2 |
|
-βzγ |
( γ-1)(βzβx/β)2 |
( γ-1)(βzβy/β)2 |
1+( γ-1)(βz/β)2 |
General Lorentz Boost Transform using
just vectors & components-Thank you Jackson, Master of Vectors!
Chap. 11
β = v/c, β = |β|, γ
= 1/√[1-β2]
a0' = γ(a0-β·a)
a'
= a+(β·a)β(γ-1)/β2-γ
β a0
a0' = γ(a0-β·a)
Temporal component
a||' = γ(a||-βa0)
Spatial parallel component
a⊥' = a⊥
Spatial perpendicular components
We are also able to use
the Rapidity
φ = Ln[γ(1+ β)] = Rapidity (which remains strictly additive in SR, unlike v)
φ = aTanh[|p|c/E] = (1/2) Ln[(E+|p|c)/(E-|p|c)]
eφ =
γ(1+β) = √[(1+β)/(1-β)]
β =
Tanh[φ], γ = Cosh[φ], γβ = Sinh[φ]
φAC =
φAB +
φBC,
Rapidity of C wrt. A = Rapidity of B wrt. A + Rapidity of C wrt. B, provided that A,B,C are co-linear
i.e. Rapidity is strictly additive only for co-linear points
Λuv = (for x-boost, y & z unchanged)
|
Cosh[φ] |
-Sinh[φ] |
0 |
0 |
|
-Sinh[φ] |
Cosh[φ] |
0 |
0 |
|
0 |
0 |
1 |
0 |
|
0 |
0 |
0 |
1 |
Rz = (for x-y rotation about z-axis, t & z unchanged)
|
1 |
0 |
0 |
0 |
|
0 |
Cos[φ] |
-Sin[φ] |
0 |
|
0 |
Sin[φ] |
Cos[φ] |
0 |
|
0 |
0 |
0 |
1 |
Time t = γ to --> Time Dilation (e.g.
decay times of unstable particles increase in a cyclotron)
Length
L = Lo/γ --> Length Contraction
A few 4-vectors are known to have complex components. The
Polarization 4-vector and Probability Current 4-vector are a couple of
these.
It will be assumed that all
physical 4-vectors may potentially be complex, although, as far as I
know, these only come into play via QM...
i = √[-1]
:Imaginary Unit
e0: Unit vector in the
temporal direction (typically not used since the temporal unit is
always considered a scalar)
e1, e2,
e3 :Unit Vectors in the spatial x, y, z
directions (used instead of i, j, k so that
there is no confusion with the imaginary unit i)
Note that for
the following 4-vectors, the superscript is the tensor index, not
exponentiation.
A = (a0c + a1c
e1+ a2c e2+
a3c e3): Complex
4-vector has complex components, 1 along time and 3 along space
Scalar[A] = a0c: Just the time
component
Vector[A] = a1c e1
+ a2c e2 + a3c
e3: Just the spatial components
A
= Scalar[A] + Vector[A]
A = (
(a0r + a0i ) +
(a1r + a1i ) e1
+ (a2r + a2i
) e2 + (a3r
+ a3i ) e3 ):
Complex 4-vector has real + imaginary components, 1 each along time
and 3 each along space
Re[A] = (
(a0r ) + (a1r
) e1 + (a2r
) e2 + (a3r
) e3 ): Only
the real components
Im[A] = (
(a0i ) + (a1i
) e1 + (a2i
) e2 + (a3i
) e3 ): Only
the imaginary components
A = Re[A] + i Im[A]
A
= (a0r + i a0i,ar
+ i ai) : Standard 4-vector
A*
= (a0r - i a0i,ar
- i ai): Complex conjugate 4-vector, just changes
the sign of the imaginary component
A = (a0r
+ i a0i,ar + i ai)
: A* = (a0r - i a0i,ar
- i ai)
B = (b0r +
i b0i,br + i bi)
: B* = (b0r - i b0i,br
- i bi)
A·B = [(
a0r b0r - ar·br
) - ( a0i b0i - ai·bi
)] + i [( a0r
b0i - ar·bi
) + ( a0i b0r - ai·br
)] : General scalar product
A·A =
[( a0r2
- ar·ar ) - ( a0i2
- ai·ai )]
+ 2i
[( a0r
a0i - ar·ai )] = |A|2 : Scalar product of
4-vector with itself
gives the magnitude squared
A·A* = [(
a0r2 + a0i2
) - ( ar·ar + ai·ai
)] = Re[A·A*]: Scalar
product of 4-vector
with its complex conjugate is Real, thus Im[A·A*]
= 0
∂·B = [( ∂/c∂tr
b0r + delr·br
) - ( ∂/c∂ti b0i + deli·bi
)] + i [(
∂/c∂tr b0i +
delr·bi ) + ( ∂/c∂ti
b0r + deli·br
)]
= [( ∂/c∂tr b0r
+
delr·br ) - ( ∂/c∂ti
b0i + deli·bi
)]
= Re[∂·B]
The 4-Divergence of a Complex
4-Vector is Real, assuming that:
The real gradient acts only on
real spaces & the imaginary gradient acts only on imaginary
spaces, thus Im[∂·B] = 0
I believe this is due
to the physical functions being complex analytic functions.
i = √[-1] :Imaginary Unit
π = 3.14159265358979...
:Circular Const
c = Speed of Light Const =
1/√[εoµo] ~ 2.99729x108
[m/s]
h =
Planck's Constant - relates particle to wave - Action constant
hbar =
(h/2π) = Planck's Reduced Const , aka. Dirac's Const - same idea
as transforming between cycles and radians for angles
In essence,
the reduced Planck constant is a conversion factor between phase (in
radians) and action (in joule-seconds)
kB = Boltzmann's
Const ~ 1.3806504(24)×10−23 [J/ ŗK]
relates temperature to energy
mo = Rest Mass Const
(varies with particle type)
q = Electric Charge Const
(varies with particle type)
Note:
I do not
set various fundamental physical constants to dimensionless unity,
(i.e. c = h = G = kB = 1).
While doing so may make the
mathematics/geometry a bit easier, it ultimately obscures the
physics.
While pure 4-Vectors may be Math, SR 4-Vectors is
Physics. I prefer to keep the dimensional units.
Also, it is much easier to set them to unity in a final formula than to figure
out where they go later if you need them.
|
4-Vector Name |
4-Vector Components |
Units (mksC) - Description |
| |
|
|
| |
|
|
|
4-Displacement |
ΔR = (cΔt, Δr) |
[m], Δt = Temporal Displacement, Δr
= Spatial Displacement, (Finite Differences) |
|
4-Differential |
dR = (cdt, dr) |
[m], dt = Temporal Differential, dr
= Spatial Differential, (Infinitesimals) |
|
4-Gradient |
∂ = ∂/∂xμ =
(∂/c∂t, -del) = (∂/c∂t, -∇) |
[m-1], ∂ is the partial
derivative, -del = -(∂/∂x i + ∂/∂y
j + ∂/∂z k) is the negative gradient operator |
|
4-MomentumGradient?? |
∂p= ∂/∂pμ =
(c∂/∂E, -delp)?? |
[kg-1 m-1 s], ∂p is the
momentum-space partial
derivative, -delp =
negative momentum-space gradient |
| |
|
|
| |
|
|
|
4-Position |
R = Rμ = (ct, r),
eg. radial coords |
[m], t = Time (temporal), r or x
= 3-Position (spatial) |
|
4-Velocity |
U = dR/dτ |
[m s-1], γ = relativistic
factor, ur
= Relativistic 3-Velocity, u = dr/dt = Newtonian
3-Velocity |
|
4-Acceleration |
A = dU/dτ |
[m s-2], ar
= Relativistic 3-Acceleration, a = du/dt = Newtonian
3-Acceleration ar = (γur)' = γ' ur + γ ur' = γ' u + γ a = (γ3/c2)(u·a) u+γ a a = du/dt = u' γ' = dγ/dt = (γ3/c2)(u·a) = ar·u/c2 Interesting note: The temporal component has units of frequency, before the c factor, and is given by γ(dγ/dt)=γ(γ') γ(c γ')=γ(ar·u/c) γ'=(ar·u/c2) 4-Spin also has a temporal component in this form, given by u·s/c I now wonder if all 4-vectors which are tangent to the worldline possess this "cyclic" feature... |
|
4-Jerk |
J = dA/dτ |
[m s-3], jr
= Relativistic 3-Jerk, j = da/dt = Newtonian
3-Jerk |
|
4-Snap |
S = dJ/dτ |
[m s-4], sr
= Relativistic 3-Snap, s = dj/dt = Newtonian 3-Snap |
| |
|
|
| |
|
|
|
4-Momentum |
P = moU
= (Eo/c2)U
= hbarK |
[kg m s-1],
E = Energy,
pr
= Relativistic 3-Momentum, p = mdr/dt = Newtonian
3-Momentum |
|
4-MomentumDensity |
G = (u/c, g) = (pmc,
g) = po_m γ(c, u) |
[kg m-2 s-1], u
= EnergyDen = ne, pm = MassDen = u/c2 |
|
4-Force |
F = dP/dτ |
[kg m s-2], dE/dt = Power, fr
= Relativistic 3-Force, f
= Newtonian 3- Force |
|
4-Force Density |
Fd = F/Vo or F/δVo Fd = γ(du/cdt, fdr) = dG/dτ?? |
[kg m-2 s-2],
4-Force divided by rest volume element |
| |
|
|
| |
|
|
|
4-WaveVector |
K = (1/hbar)P = (mo/hbar)U
= (ωo/c2)U |
[rad m-1], ω =
AngularFrequency [rad/s], k = WaveNumber or WaveVector
[rad/m] |
|
4-Frequency |
Ν =
(ν, c/λ n) |
[cyc s-1], ν = ω/2π,
λ = 2π/k |
|
4-CycWaveVector |
Kcyc = (ν/c,1/λ n) |
[cyc m-1], ν =
CyclicalFrequency [cyc/s], λ = WaveLength [m/cyc] |
| |
|
|
| |
|
|
| |
|
|
|
4-NumberFlux |
N = (cn, nf)
= no γ(c, u) = n(c, u) |
[(#) m-2 s-1], no
= RestNumberDensity [#/m3], n = γno =
NumberDensity [#/m3] |
|
4-VolumetricFlux |
V = VoU?? |
[(m3) m-2 s-1],
Vo = RestVolume |
|
4-ElectricCurrentDensity |
J = (cρ, j) = ρo
γ(c, u) = ρ(c, u) |
[(C) m-2 s-1], ρo
= RestElecChargeDensity [C/m3], ρ = γρo
= ElecChargeDensity |
|
4-MagneticCurrentDensity |
Jmag = (cρmag,
jmag) = ρo_mag γ(c,
u) |
[(MagCharge) m-2 s-1],
ρo_mag = RestMagChargeDensity, ρmag
= γρo_mag = MagChargeDensity |
|
4-ChemicalFlux |
|
[(mol) m-2 s-1], |
|
4-MassFlux |
G = (u/c, g) = (cρm,
g) = ρo_m γ(c, u) = ρo_mU |
[(kg) m-2 s-1], u
= EnergyDen = ne, pm = MassDen = u/c2 |
|
4-PoyntingVector |
S = (cu, s) = uo
γ(c, u) = uoU = c2G |
[(J) m-2 s-1], u
= EnergyDen = ne, s = EnergyFlux = PoyntingVector = uu
= c2g = Ne |
|
4-EntropyFlux |
S = (cs, sf) |
[(J ŗK-1)
m-2
s-1],
so
= RestEntropyDensity = qo/T,
sf
= EntropyFlux |
| |
|
|
| |
|
|
|
4-InverseTempFlux |
β =
βo
U
= (1/kBTo)
U |
Considered on Thermodynamic
principles |
|
4-MomentumTemperature |
PT = P/kB
= (pT0/c, pT) =
(T/c, pT) = ((E/kB)/c, p/kB)
|
[ŗK m-1 s], |
| |
|
|
| |
|
|
|
4-Potential Flux?? |
V =
(cq, qf)
= q
γ(c, u)
= qU?? |
Potential Flow for Velocity?? In fluid dynamics, a potential flow is described by means of a velocity potential , φ being a function of space and time. The flow velocity v is a vector field equal to the negative gradient, del, of the velocity potential φ: Incompressible flowIn case of an incompressible flow — for instance of a liquid, or a gas at low Mach numbers; but not for sound waves — the velocity v has zero divergence: del·v = 0with the dot denoting the inner product. As a result, the velocity potential φ has to satisfy Laplace's equation del·del φ = 0where Δ = ∇·∇ is the Laplace operator. In this case the flow can be determined completely from its kinematics: the assumptions of irrotationality and zero divergence of the flow. Dynamics only have to be applied afterwards, if one is interested in computing pressures: for instance for flow around airfoils through the use of Bernoulli's principle. The flow velocity of a fluid effectively describes everything about the motion of a fluid. Many physical properties of a fluid can be expressed mathematically in terms of the flow velocity. Some common examples follow: Steady flowMain article: Steady
flow Incompressible flowMain article: Incompressible
flow Irrotational flowMain article: Irrotational
flow VorticityMain article: Vorticity
The velocity potentialMain article: Potential
flow An lamellar vector field is a synonym for an irrotational vector field.[1] The adjective "lamellar" derives from the noun "lamella", which means a thin layer. In Latin, lamella is the diminutive of lamina (but do not confuse with laminar flow). The lamellae to which "lamellar flow" refers are the surfaces of constant potential. An irrotational vector field which is also solenoidal is called a Laplacian vector field. The fundamental theorem of vector calculus states that any
vector field can be expressed as the sum of a conservative vector
field and a solenoidal field. The fundamental theorem of vector calculus states that any
vector field can be expressed as the sum of a conservative vector
field and a solenoidal field. The condition of zero divergence is
satisfied whenever a vector field v has only a vector
potential component, because the definition of the vector
potential A as: automatically results in the identity (as can be shown, for
example, using Cartesian coordinates): The converse also holds: for any solenoidal v there exists a vector potential A such that v = del x A. (Strictly speaking, this holds only subject to certain technical conditions on v, see Helmholtz decomposition.) In vector calculus, a Laplacian vector field is a
vector
field which is both irrotational and incompressible. If the field
is denoted as v, then it is described by the following
differential equations: Since the curl of v is zero, it follows that v
can be expressed as the gradient of a scalar potential (see
irrotational field) φ : Then, since the divergence of v is also zero, it follows from equation (1) that del·del φ = 0 which is equivalent to Therefore, the potential of a Laplacian field satisfies
Laplace's equation. In case of an incompressible flow the velocity potential satisfies the Laplace's equation. However, potential flows have also been used to describe compressible flows. The potential flow approach occurs in the modeling of both stationary as well as nonstationary flows. Applications of potential flow are for instance: the outer flow field for aerofoils, water waves, and groundwater flow. For flows (or parts thereof) with strong vorticity effects, the potential flow approximation is not applicable. A velocity potential is used in fluid dynamics, when a
fluid occupies a simply-connected region and is irrotational. In
such a case, where u denotes the flow velocity of the fluid. As a
result, u can be represented as the gradient of a scalar
function Φ: Φ is known as a velocity potential for u. A velocity potential is not unique. If a is a constant then Φ + a is also a velocity potential for u. Conversely, if Ψ is a velocity potential for u then Ψ = Φ + b for some constant b. In other words, velocity potentials are unique up to a constant. Unlike a stream function, a velocity potential can exist in three-dimensional flow. |
|
4-HeatFlux |
Q = qU |
[(J) m-2 s-1] =
[(W)
m-2], |
|
4-DarcyFlux |
Q = (cq, qf)
= q γ(c, u) = qU
=
( c (βφ)P , qf) |
[(m3)
m-2
s-1]
= [m s-1], |
|
4-ElectricChargeFlux |
Q = (cq, qf) = q γ(c, u) = qU = ( c ρ, j) |
[(C) m-2
s-1], |
| |
|
|
| |
|
|
|
4-SpinMomentum |
W =
(w0,w)
= (u·w/c,w) |
[spin-momentum], |
|
4-Spin |
S =
(s0,s)
= (u·s/c,s) |
[ J s], = [spin] Spin =
IntrinsicAngMomentum, u·s/c
= component such that U·S = 0 |
|
4-SpinDensity |
|
|
|
4-Polarization |
Ε =
(ε0,
ε)
= (ε·u/c,ε)
for a massive particle |
[1], ε = PolarizationVector
**This 4-vector has complex components in QM** |
|
4-SpinPolarization |
In the rest frame, where K
= (m,0),
choose a unit 3-vector n
as the quantization axis. |
|
|
4-PauliMatrix |
Σ = Σμ =
(σ0, σ) |
The components of this 4-vector are actually the Pauli Matrices |
| |
|
|
| |
|
|
|
4-VectorPotential |
A = (Φ/c,
a) |
[kg m <chargetype>-1
s-1],
for arbitrary field |
|
4-VectorPotentialMomentum |
QEM
= (EEM/c,
pEM) |
[kg m s-1], |
|
4-Potential |
ΦEM = (ΦEM,c
aEM) |
[kg m2 C-1 s-2],
ΦEM = ScalarPotenialEM ,aEM
= VectorPotenialEM |
|
4-MomentumEM |
PT
= (ET/c + qΦEM/c,
pT +
qaEM) |
[kg m s-1], **Momentum
including effects of potentials** H = γmoc2
+ q ΦEM |
|
4-GradientEM |
DEM
= (∂/c∂t + iq/hbar
ΦEM/c,
-del
+ iq/hbar
aEM) |
[m-1], **Gradient including
effects of EM potentials** |
| |
|
|
| |
|
|
|
4-Differential |
dX = (cdt, dx) |
[m], dt = Temporal Differential, dx = Spatial Differential |
|
4-Volume Element (Flux?) |
dV = (c dv0,dv) |
[m3], A vector-valued volume
element is just a 4-vector that is perpendicular to all spatial
vectors in the volume element, and has a magnitude that's
proportional to the volume. |
|
4-Momentum Differential |
dP = (dE/c, dp) |
[kg m s-1], dE = Temporal Momentum Differential, dp = Spatial Momentum Differential |
|
4-MomentumSpace |
dVp = (c
dvp0,dvp) |
[kg3 m3 s-3],
A vector-valued MomentumSpace volume element is just a 4-vector
that is perpendicular to all spatial vectors in the MomentumSpace
volume element, and has a magnitude that's proportional to the
MomentumSpace volume. |
| |
|
|
| |
|
|
|
4-Zero |
Zero = (0,0) = (0,0,0,0) |
[*], All components are 0 in all
reference
frames, the only vector with this property |
|
4-Null |
Null = (a,a) = (a,an)
= a(1,n) |
[*], Any 4-vector for which the temporal
component magnitude equals the spatial component magnitude |
|
4-Unit Temporal |
T = (1,0) |
[*], The Unit Temporal 4-Vector |
|
4-Unit Null |
N = (1,n) |
[*], The Unit Null 4-Vector |
|
4-Unit Spatial |
S = (0,n) |
[*], The Unit Spatial 4-Vector |
|
4-Basis Vectors |
Bt =
(1,0,0,0) |
A tetrad of 4 mutually orthogonal,
unit-length, linearly-independent, basis vectors |
|
4-Basis Vectors |
Bn1 = √[1/2]
(1,0,0,1) |
A tetrad of unit-length,
linearly-independent, null basis vectors |
|
4-ProbabilityCurrentDensity |
Jprob = (cρ, j)
= (ihbarρo/mo)(ψ*<-∂->ψ)/2 |
[# m-2 s-1],
4-Probability
Current Density is proportional to the 4-Momentum |
Event Tracking Relations
|
Event R |
Mass
mo = ρo_mVo |
WaveAngFreq ωo |
ElecCharge q = ρoVo |
MassDensity ρo_m |
ChargeDensity ρo |
NumberDensity no
|
|
event |
particle |
wave |
elec. charge |
mass |
charge |
number |
|
pos: R = (ct, r) |
mo at R |
ωo at R |
q at R |
ρo_m at R |
ρo at R |
no at R |
|
vel: U = dR/dτ |
P = moU = (Eo/c2)U |
K = (ωo/c2)U = (1/hbar)P |
Jq = qU |
G = ρo_mU = (uo/c2)U |
J = ρoU |
N = noU |
|
accel: A = dU/dτ |
F = dP/dτ |
|
|
Fd = dG/dτ |
|
|
|
jerk: J = dA/dτ |
|
|
|
|
|
|
| snap: S = dJ/dτ |
∂·R = (∂/c∂t,-del)·(ct,r)
= (∂/c∂t[ct]+del·r) = (∂/∂t[t]+del·r)
= (1+3) = 4
∂·R = 4 The divergence of
open spacetime is equal to the number of independent dimensions (1
time + 3 space)
d/dτ [∂·R] = d/dτ [4] = 0
d/dτ
[∂·R] = d/dτ [∂] ·
R + ∂·d/dτ [R] = d/dτ [∂] ·
R + ∂·U = γ d/dt [∂] ·
R + ∂·U = γ (d/dt[∂/c∂t], -d/dt[del])·(ct,r)
+ ∂·U
= γ (d/dt[∂/c∂t][ct]+d/dt[del])·r
+ ∂·U = γ (d/dt[∂/∂t][t]+d/dt[del])·r
+ ∂·U = γ (d/dt[1]+d/dt[3]) +
∂·U = 0 + ∂·U =
∂·U
thus,
∂·U =
0, which is the General SR Continuity Equation, one might say the
conservation of event flux or continuity of worldlines.
Due to
this property, any Lorentz scalar constant times 4-Velocity U is
a conserved quantity.
For example, let N = noU,
so ∂·N = ∂·noU =
no∂·U = no(0) = 0. The
quantity no is conserved.
Any "charge"
constant becomes a 4-vector when multiplied by the 4-Velocity, and
obeys the Conservation of Charge/Continuity equation ∂·J
= ∂ρ/∂t +del·j = 0 where J
= ρoU
let Charge q = ρoVo,
where ρo is the "rest charge density", ρ
= γρo is the relativistic "charge density",
Vo is the rest volume, and j = γρou
= ρu is the "ChargeDensity-Flux or Current
Density"
then ChargeFlux 4-Vector = CurrentDensity
4-Vector J = ρoU = ρo
γ(c, u) = ρ(c, u) = (cρ, j)
In
the case of "electric" charge, ρo is the
"rest electric-charge density", and j is the
ElectricChargedensity-flux = electric current density
In the case
of "number" charge, ρo is the "rest
number-charge density"
In the case of "mass"
charge, ρo is the "rest mass density", and j
is the mass-flux = mass current density = momentum density
Poincaré
transformation or an inhomogeneous Lorentz transformation:
ημν
Λμα Λ νβ
= ηαβ
Chain rule on the
4-gradient:
Let gμ = ∂μ f = ∂f
/ ∂xμ
Using the chain rule, one can show:
g'ν
= ∂f '/∂x'ν = Σ ( ∂f / ∂xμ
)( ∂xμ / ∂x'ν ) = ∂'ν
f ' = ( ∂μ f )( ∂'ν xμ
) = (gμ)( ∂'ν xμ
)
where the brackets indicate that the gradient acts only on the
function inside the given bracket
However, this appears to be a
standard Lorentz transform
∂'μ = Λμν
∂ν[function argument] = ∂ν[function
argument] Λμν
Let ∂'·J'
= ∂ρ'/∂t +del·j' = 0 be an
arbitrary 4-vector continuity equation.
∂'·J'
= ημν ∂'μ J'ν =
ημν Λμα ∂α
J'ν = ημν Λμα
∂α Λνβ Jβ
= ημν Λμα
Λνβ ∂α Jβ
= ηαβ ∂α Jβ
= ∂·J
Assuming that the 4-gradient acts only on
the 4-vector J, and not on the metric and Lorentz transforms,
which
appears to be the case based on the chain rule
So, ∂'·J'
= ∂·J, the continuity equations holds in arbitrary
inertial reference frames
Consider a scalar ( s ) and a vector
( v ) related by a continuity equation, ∂s/∂t +del·v
= 0.
If this equation holds in all inertial reference frames, then
s and v must be components of a 4-vector (cs, v).
see
http://www.grc.nasa.gov/WWW/K-12/Numbers/Math/Mathematical_Thinking/proposed_relativistic.htm
|
Event(SR) |
EventMovement |
MassEnergy |
Particle-WaveDuality |
QuantumMechanics(QM) |
SpaceTimeVariations |
|
R = (ct, r) |
dR/dτ = U = γ(c,u) |
U = P/mo |
P = hbar K |
*** K = i ∂ *** |
∂ = (∂/c∂t,-del) |
| |
|
|
or K = (ωo/c2)U |
|
|
d/dτ[R] = (i hbar
/ mo) ∂ Event motion ~ spacetime structure -
depends on i hbar / mo
So,
the following assumptions within SR-Special Relativity lead to
QM-Quantum Mechanics:
|
R = (ct,r) |
Location of an event (i.e. a particle) within spacetime |
|
U = dR/dτ |
Velocity of the event is the derivative of event position wrt. Proper Time |
|
P = moU |
Momentum is just the Rest Mass of the particle/event times its velocity |
|
K = (1 / hbar )P |
A particle's wave vector is just the momentum divided by Dirac's constant, but uncertain by a phase factor |
|
∂ = -i K |
The change in spacetime corresponds to (-i) times the wave vector, whatever that means... |
R·R = (Δ s)2
= (ct)2-r·r = (ct)2-|r|2
: dR·dR = (ds)2 = (c dt)2-dr·dr
= (c dt)2-|dr|2 : Invariant
Interval
U·U = c2
P·P
= (moc)2
K·K = (moc
/ hbar)2 = (ωo/c)2
∂·∂
= (∂/c∂t,-del)·(∂/c∂t,-del)
= ∂2/c2∂t2-del·del
= -(moc / hbar)2 : Klein-Gordon
Relativistic Wave Eqn.
Each relation may seem simple, but there is
a lot of complexity generated by each level.
*see QM
from SR (Quantum Mechanics derived from Special
Relativity)*
This can be further explored:
∂·∂
+ (moc / hbar)2 = 0
|
(∂·∂ + (moc / hbar)2 ) Ψ = 0, |
Ψ is a scalar Klein-Gordon eqn for massive spin-0 field |
|
(∂·∂ + (moc / hbar)2 ) A = 0 |
A is a 4-vector Proca eqn for massive spin-1 field |
|
(∂·∂) Ψ = 0 |
Ψ is a scalar Free-wave eqn for massless (mo = 0) spin-0 field |
|
(∂·∂) A = 0 |
A is a 4-vector Maxwell eqn for massless (mo = 0) spin-1 field, no current sources |
Interesting Note about Proca
eqn.
"Massive charged vector field - represent with complex
four-vector field φμ(X) and impose "Lorenz
condition" (∂μφμ) = 0 so
that φ0(X) -the scalar polarization- , can be
discarded and the Klein-Gordon equations emerge for the other three
components φi(X)
(∂·∂
+ (moc / hbar)2 ) A = 0,
where A is a 4-vector Proca eqn for massive spin-1
field
rewrite in index notation
(∂μ∂μ
+ (moc / hbar)2 ) Aν =
0 and combine with the Lorenz gauge condition (∂μAμ
= 0)
apparently, this conjunction is equivalent to
∂μ(
∂μ Aν - ∂ν Aμ
)+ (moc / hbar)2 Aν
= 0
which is the Euler-Lagrange equation for the Proca Action
see
Conceptual Foundations of Modern Particle Physics, ~ pg. 100
Momentum/Gradient Relations(Correspondences)
|
P = i hbar ∂ = -∂(Sact) |
∂ = (∂/c∂t,-del) |
AEM = (0,0) *special case* |
|
PEM = P+qAEM = i hbar DEM |
DEM = ∂+iq/hbar AEM |
AEM = (VEM/c,aEM) |
| |
Relations involving the 4-Position or 4-Displacment: |
|
R·R = (Δs)2 = (ct)2-r·r
= (ct)2-|r|2 |
Spacetime position of an event wrt. an origin event |
|
dR·dR = (ds)2 |
Differential interval magnitude - the
fundamental invariant differential form |
|
ΔR·ΔR = (Δs)2 = (c Δt)2-Δr·Δr = (c Δt)2-|Δr|2 |
Spacetime displacement interval
magnitude
- used to derive SR |
|
∂·R = 4 |
The divergence of open spacetime is equal to the number of independent dimensions (t,x,y,z) |
|
K·R = -φEM = (ωt-k·r) |
Phase of a SR wave; Ψ = a E e -iK·R Photon Wave Equation (Solution to Maxwell Equation) |
|
R·U = (ct,r)·γ(c,u ) = γ(c2t - r·u) |
Part of expression used in Liénard-Wiechert potential |
| |
|
| |
Relations involving the 4-Velocity: |
|
U·U = c2 |
The magnitude of 4-Velocity is always c2 |
|
U1·U2
= γ[u1]γ[u2](c2-u1·u2)
= γ[urel]c2 |
Relative Gamma Factor |
|
A1·U1 = 0, where A is dU/dτ |
The 4-Acceleration of a given particle is always normal to its own worldline |
|
P1·U2
= γ[u2](E-p1·u2)
= Erel |
Relative Energy |
|
K1·U2
= γ[u2](ω-k1·u2)
= ωrel |
Relative Ang. Frequency |
|
F·U = (moA+(dmo/dτ)U)·U
= c2(dmo/dτ) = γc2(dmo/dt) |
Power Law |
|
U·∂ = γ(∂/∂t + u·del) = γ d/dt = d/dτ |
Relativistic Convective (Time)
Derivative, Intrinsic Derivative |
|
∂·U = 0 (always??) |
The General Continuity Equation, one
might say the conservation of event flux. |
| |
|
| |
Relations involving the 4-Acceleration: |
|
A·A = -a2 = -γ4[a2 + (γ/c)2(u·a)2] |
Magnitude squared of acceleration |
|
U·A = 0, where A is dU/dτ |
The 4-Acceleration of a given particle
is always normal to
its own worldline |
| |
|
| |
Others: |
|
P·P = (moc)2 =
(Eo/c)2 |
Square Magnitude of the 4-Momentum |
|
P1·P2
= γ[u1]γ[u2]mo1
mo2(c2-u1·u2) |
Relativistic Billiards... |
|
N·N = (noc)2 |
Square Magnitude of the 4-NumberCurrentDensity |
|
J·J = (poc)2 = (qnoc)2 |
Square Magnitude of the 4-ElectricCurrentDensity |
|
K·K = (moc / hbar)2
= (ωo/c)2 |
Square Magnitude of the 4-WaveVector |
|
∂·∂ = (∂/c∂t,-del)·(∂/c∂t,-del) = ∂2/c2∂t2-del·del = -(moc / hbar)2 |
Klein-Gordon Relativistic Wave Eqn. |
|
∂·J = ∂ρ/∂t +del·j = 0 |
Continuity Equation - Conservation of
Electric Charge |
|
E·K = 0 |
The Polarization of a photon is orthogonal to direction of wave motion (cancellation of "scalar" polarization) |
|
E·E* = -1 |
The Polarization of a photon is always unit magnitude and space-like (cancellation of the longitudinal polarization) |
|
AEM·AEM = (VEM/c,aEM)·(VEM/c,aEM) = (VEM/c)2-aEM·aEM = ???? |
Square Magnitude of the Electromagnetic field |
There is an important distinction between an invariant quantity
and a conserved quantity.
An invariant quantity has the same
value wrt. all inertial systems, but may change upon physical
interaction (e.g. a fission/fusion reaction "redistributes"
the rest masses).
A conserved quantity maintains the same value
both before and after an interaction, although the component values
may appear different in different frames.
In 4-vector
notation:
An invariant quantity is a Lorentz Scalar, the dot
product of two 4-Vectors, A·B = invariant = same
value for all inertial observers.
A conserved quantity is a
component of a 4-Vector that has 4-Divergence = 0, ∂·V
= 0.
Relativistic Invariant
Quantities
(Lorentz Scalars~A·B), although perhaps there might be
some
that are simply just scalars...
also known as Relativistic Covariance
Lorentz Scalars = World Scalars = Invariant Scalars
|
c = √[U·U] |
Speed of Light: c (in vacuum) E ~ cp |
||
|
h = √[P·P/L·L]
= P·L / L·L |
Planck's const: h, E ~ hν |
||
|
kB = √[P·P/PT·PT] = P·PT / PT·PT |
Boltzmann's const: kB, E ~ kBT |
||
|
|
|
||
|
γrel = V·U / U·U |
Relative Relativistic Gamma Factor, between 4-velocities U and V |
||
| |
|
||
|
Δs = √[ΔR·ΔR] = √[c2Δt2 - Δx2 - Δy2 - Δz2] |
Displacement |
||
|
Δσ = √[-ΔR·ΔR] = √[-(c2Δt2 - Δx2 - Δy2 - Δz2)] |
Proper Distance, for SpaceLike Intervals |
||
|
ds = √[dR·dR] = √[c2dt2 - dx2 - dy2 - dz2] ds2 = dR·dR = c2dt2 - dx2 - dy2 - dz2 |
Differential Length of World Line
Element, the SpaceTime Interval ds |
||
|
dτ = √[dR·dR/U·U] |
Differential Proper Time, aka. the Eigentime differential |
||
|
d/dτ = U·∂ =
γ(∂/∂t + u·del) |
Derivative wrt Proper Time d/dτ |
||
|
Δ = ∂·∂ =
(∂/c∂t,-del)·(∂/c∂t,-del) |
D'Alembertian/wave operator |
||
|
d4x |
Invariant 4-volume |
||
|
d4p = dP·dVp |
Spacetime momentum-space differential "4-volume" element |
||
|
d4k = dK·dVk |
Spacetime wavevec-space differential "4-volume" element?? |
||
|
d3xd3p = dV = dμ[t] = dV·dVp |
Invariant phase volume |
||
|
δ4(x-y) |
4-D Dirac Delta Function |
||
|
G(x|x') |
Green's Function where ∂·∂
G(x|x') = δ4(x-x') |
||
|
f(t,x,p) |
One Particle Distribution Function |
||
| N[t] = f(t,x,p) dμ[t] | Number of particles in a volume element | ||
|
d3p/(2E) |
Invariant phase-space element |
||
| d3p/(2E) = p2dpdΩ/(2E) | Spacetime phase-space differential
3-volume element, cartesian vs. spherical basis dΩ = Solid Angle Element in direction of Ω |
||
| (2E)δ3(p-p'), (2ω)δ3(k-k') |
Spacetime phase-space differential
3-volume element, Dirac form need to get exact units, etc. corrected δ4(p-p') => Lorentz Invariant δ( E - Eo )δ3(p-p') δ( E - Eo )δ3(p-p') / δ( F[E] ) Divide by another Lorentz invariant δ( E - Eo )δ3(p-p') / δ( E - Eo )/|2E| δ( E - Eo ) |2E| δ3(p-p') / δ( E - Eo ) |2E| δ3(p-p') |
||
| u[ε,Ω]/ε3 | Specific spectral energy density over dimensionless energy cubed | ||
| Iε[Ω]/ε3 | Intensity over dimensionless energy cubed | ||
| j[ε,Ω]/ε2 | Emissivity over dimensionless energy squared |
||
|
mo = √[P·P/U·U] = P·U/U·U |
RestMass of a Particle mo ( 0 for photons, + for massive ) |
||
|
ρo = mono = (rest mass)*(rest number density) |
ProperMassDensity ρo of a
continuum in the co-moving frame
of no |
||
|
q = √[J·J/N·N] = J·N/N·N |
RestElectricCharge of a Particle q |
||
|
3-vector |
Spin so |
||
|
magnetic moment |
|
||
|
|
|
||
|
Eo = P·U =
moc2 |
RestEnergy of a Particle ( 0 for photons, + for massive ) |
||
|
ωo = K·U
= moc2/hbar |
RestAngFrequency of a Particle ( 0 for photons, + for massive ) |
||
|
|
|
||
|
φ = - K·R |
*** Phase of a wave ***, |
||
|
γL = - (moU·U
+ qAEM·U) |
Relativistic Lagrangian L * gamma (γ) |
||
|
L |
Lagrangian Density |
||
|
Saction = - P·R = ∫[dt L;ti,tf] |
Action Variable S of Action Integral |
||
| H / γ = PT·U |
Relativistic Hamiltonian H / gamma (γ) Start with Lagrangian L[qi,qi'], a function of coords qi and their time derivatives qi' Conjugate momenta pi = ∂L/∂qi' Then Hamiltonian H = Σ [piqi';i] - L Then, Eqns. of Motion p' = -∂H/∂q q' = ∂H/∂p ex. Lagrangian of a free particle L = -moc2/γ pi = ∂L/∂qi' = γmoui (or p = γmou) H = Σ [piqi';i] - L = p·u - L = γmou·u + moc2/γ = γmoc2 where γ2 = c2/(c2-v2) = c2/(c2-u·u) p' = -∂H/∂q = 0, since H = γmoc2 has no explicit dependence on q q' = ∂H/∂p = u So, p' ~ a = 0 ie. no acceleration q' = u as we expect Hamiltonian for a free particle: H = γmoc2 = E ; H/γ = moc2 = Eo ------- ex. Lagrangian of a charged particle in EM field
L = -(P + QEM)·U/γ L = -(P·U + QEM·U)/γ L = -P·U/γ - QEM·U/γ L = -moU·U/γ - qAEM·U/γ L = -moc2/γ - qAEM·U/γ L = -moc2/γ - q(ΦEM/c, aEM)·γ(c, u)/γ L = -moc2/γ - q(ΦEM/c, aEM)·(c, u) L = -moc2/γ - q(ΦEM - aEM·u) L = -moc2/γ - qΦEM + qaEM·u L = -moc2/γ - qΦoEM/γ L = -(moc2 + qΦoEM)/γ pcanonical = ptotal = ∂L/∂q' = (γmou) + (qaEM) = (pdynamical) + (qaEM) = (pkinetic) + (ppotential) Hence, γmou = p - qaEM Equation of motion: (leading to negative gradient of potential) dp/dt = ∂L/∂x = - q(∂ΦEM/∂x - ∂aEM/∂x·u)
H = ptotal·u - L H = γmou·u + qaEM·u - L H = γmou·u + qaEM·u + moc2/γ + q(ΦEM - aEM·u) H = γmou·u + moc2/γ + q(ΦEM) H = p·u + moc2/γ + q(ΦEM) H = γmoc2 + qΦEM H = E + V = (rest+kinetic) + (potential) H = moc2 + (γ-1)moc2 + qΦEM H = (rest) + (kinetic) + (potential) also, since E=√[p·p c2 + mo2c4] H = √[ptotal2c2 + mo2c4] + qΦEM H = √[(pkinetic - qaEM)2 c2 + mo2c4] + qΦEM q' = ∂H/∂p = (p - qaEM) / √[(p - qaEM)2 /c2 + mo2] p' = -∂H/∂q = q(del aEM) ·u - qdelΦEM this leads to the Lorentz force (here E and B are the classical electric and magnetic fields, not 4-vectors): ptotal' = f = q(E + v x B) representing the rate at which the EM field adds relativistic momentum to a charged particle dp/dτ = γq(E + v x B) The non-relativistic Lagrangian L is an approximation of the relativistic one: L = -(moc2 + qΦoEM)/γ -L = (moc2 + qΦoEM)/γ = √[1-(v/c)2](moc2 + qΦoEM) ~ (moc2 + qΦoEM) - (1/2)(moc2v2/c2 + qΦoEMv2/c2) ~ (moc2 + qΦoEM) - (1/2)(mov2 + 0) L ~ (1/2)(mov2) - (moc2 + qΦoEM) L ~ (Kinetic) - (Rest+Potential) = T - V (for v << c) The large constant coming from the restmass is simply ignored in classical mechanics. The gamma factor in the Lagrangian corresponds to the time dilation of an object moving at v. In QM words: the number of phase changes (ticks) over the trajectory of the particle (the t' axis) is less by a factor gamma. The non-relativistic Hamiltonian H is an approximation of the relativistic one: H = γ(moc2 + qΦoEM) H = (1/√[1-(v/c)2])(moc2 + qΦoEM) ~ [1+(v/c)2/2])(moc2 + qΦoEM) = (moc2 + qΦoEM)+(1/2)(moc2v2/c2 + qΦoEMv2/c2) ~ (moc2 + qΦoEM) -+(1/2)(mov2 + 0) H ~ (1/2)(mov2) + (moc2 + qΦoEM) H ~ (Kinetic) + (Rest+Potential) = T + V (for v << c) In QM words: the number of phase changes (ticks) over the t axis is higher by a factor gamma. Thus, L ~ T-V and H ~ T+V only in the non-relativistic limit (v<<c) |
||
|
T = (1/2)moU·U= (1/2)P·U |
Relativistic Kinetic Energy Term T |
||
|
ψ , ψ* |
Scalar Quantum Wave Function |
||
| |
|
||
| |
|
||
|
no = √[N·N/U·U] = N·U/U·U = n/γ |
Particle RestNumberDensity (for stat mech) |
||
|
so = √[S·S/U·U] = S·U/U·U |
RestEntropyDensity (for stat mech) |
||
|
|
|
||
|
Ωo = Ω |
Ω = # of microstates = (N!) / (n0!n1!n2!...) |
||
|
No = N |
(Stable) Particle Number: N = nV =
(n/γ)(γ V) = noVo = No |
||
|
Po = P |
Pressure of system: P = Po |
||
|
So = S = kB ln Ω |
Entropy: S = sV = (s/γ)(γ V) = soVo = So , |
||
|
To = γ T |
RestTemperature (according to Einstein/Planck def.) |
||
|
q = γ Q |
RestHeat |
||
|
Vo = γ V |
RestVolume |
||
|
dS = kB d(ln Ω) = δQ / T |
Change in Entropy |
||
|
|
|
||
|
Π
(pα,xα)
= |
Invariant equilibrium distribution
function for relativistic gas |
||
|
|
|
||
|
Fuv Fuv
= 2(B2 - E2/c2) |
EM invariant |
||
|
Gcd Fcd
= εabcdFabFcd
=(2/c)(B·E) |
EM invariant |
||
| P = (2q2/3c3) γ4(aperp2+
γ2a2||) P = (μoq2a2γ6)/(6πc) in parallel Generally P = μoq2(A·A)/(6πc) |
Radiated
Power P, total power is Lorentz invariant for processes with symmetry
in the rest frame |
||
| Iv/v3 |
Spectral Intensity / v3 |
||
| Helicity |
A massless particle moves with the speed of light, so a real observer (who must always travel at less than the speed of light) cannot be in any reference frame where the particle appears to reverse its relative direction, meaning that all real observers see the same chirality. Because of this, the direction of spin of massless particles is not affected by a Lorentz boost (change of viewpoint) in the direction of motion of the particle, and the sign of the projection (helicity) is fixed for all reference frames: the helicity is a relativistic invariant |
Conserved Quantities (components of V, such that the 4-Divergence ∂·V = 0 )
|
∂·J = ∂p/∂t +del·j = 0 |
Conservation of 4-CurrentDensity (EM
charge): p & j |
|
∂·N = ∂/∂t(γ
no)+del·(γ nou) |
Conservation of 4-NumberFlux (Particle
NumberDen, NumFlux): n & nf
|
|
∂·P = (1/c2)∂E/∂t
+del·p = 0 |
Conservation of 4-Momentum (Energy~Mass,
Momentum): E & p |
|
∂·K =
∂/c∂t(w/c)+del·k |
Conservation of 4-WaveVec (AngFreq,
WaveNum): w & k |
|
∂·AEM = (1/c2)∂VEM/∂t +del·aEM = 0 |
Conservation of 4-VectPotentialEM
(applies in the Lorenz Gauge): VEM & aEM
|
|
|
|
|
∂·U =
∂/∂t(γ[u])+del·(γ[u] u) |
Conservation of 4-Velocity: (Flux-Gauss'
Law)??: γ & γ u |
Lorentz 4-Tensors
|
ημν = ημν
= Diag[1,-1,-1,-1] |
Minkowski Metric (flat
spacetime) |
||||||||||||||||
|
1 if a=b, |
Kronecker Delta |
||||||||||||||||
|
= +1 if {abcd} is an even permutation of
{0123} |
Levi-Civita symbol |
||||||||||||||||
|
Fuv =
|
EM Field Tensor |
||||||||||||||||
|
Gcd = (1/2)εabcdFab =
|
Dual EM Field Tensor |
||||||||||||||||
|
Tab =
|
Energy-Momentum Stress Tensor The stress-energy tensor of a
relativistic fluid can be written in the form Here
The heat flux vector and viscous shear tensor are transverse to the world lines, in the sense that
This means that they are effectively three-dimensional quantities, and since the viscous stress tensor is symmetric and traceless, they have respectively 3 and 5 linearly independent components. Together with the density and pressure, this makes a total of 10 linearly independent components, which is the number of linearly independent components in a four-dimensional symmetric rank two tensor. |
| 4-Vector(s) |
Type |
Relativistic
Law |
Newtonian
Limit Low Velocity (v<<c) or Low Energy (E<<moc2) |
| R = (ct,r) | 4-Position |
(ct,r) is
single 4-vector entity t and r related by Lorentz transform |
t independent from r: t is independent scalar, r is independent vector |
| ΔR = (cΔt,Δr) | 4-Displacement | Relative
Simultaneity Δt' = γ(Δt - βΔr/c) |
Absolute Simultaneity Δt' = Δt |
| U = dR/dτ | 4-Velocity | Relativistic
Composition of Velocities urel = =[u1+u2]/(1+β1·β2) =[u1+u2]/(1+u1·u2/c2) |
Additive Velocities u12 = u1 + u2 |
| A = dT/dτ | 4-Acceleration | Relativistic Larmor Formula Power radiated by moving charge P = = ( q2/ 6πεoc3)(A·A) = (μoq2)/(6πc)(A·A) = (μoq2/ 6πc) γ6/ (a2 - (|u x a|)2/c2) |
Newtonian Larmor Formula Power radiated by moving charge P = (μo q2a2/ 6πc) |
| P = moU | 4-Momentum | Einstein
Energy-Mass Relation E = γ moc2 = Sqrt[ mo2c4 + p·p c2 ] |
Total Energy = Rest Energy +
Kinetic Energy E = moc2 + (p2/2mo) |
| ∂·P | Divergence of 4-Momentum | Local?
Conservation of 4-Momentum |
Conservation of Energy,
Conservation of Momentum |
| P1·P2 | Particle Interaction |
Conservation of 4-Momentum | Conservation of Energy,
Conservation of Momentum, sometimes Conservation of Kinetic Energy |
| K = 1/hbar P | 4-WaveVector | Relativistic
Doppler Effect, inc. Tranverse Doppler Effect ao_obs = = ao_emit / γ(1 - (n·v/c)) = ao_emit / γ(1 - (n·β)) = ao_emit √[1+|β|]√[1-|β|] / (1 - (n·β)) |
Regular Doppler Effect ao_obs = ao_emit √[1+|β|]√[1-|β|] |
| P and K |
4-Momentum and 4-WaveVector |
Compton Scattering (λ'-λ) = (h/moc)(1-cos[ų]) (moc2)(1/E'-1/E) = (1-cos[ų]) Ratio of photon energy after/before collision P[E,ų] = 1/[1+(E/moc2)(1-cos[ų])] see also Klein-Nishina formula |
Thompson Scattering Ratio of photon energy after/before collision: E<<moc2 P[E,ų] --> 1 |
| ∂ = -iK | 4-Gradient | D'Alembertian
& Klein-Gordon Equation ∂t2/c2 = del·del-(moc/hbar)2 |
Schroedinger Equation (i hbar)( ∂t ) = - (hbar)2(del)2/2mo |
| ∂·J
|
Divergence of 4-Current |
Conservation of
4-EM_CurrentDensity ∂·J = ∂/c∂t(cp)+del·j = ∂p/∂t +del·j = 0 |
Conservation of
4-EM_CurrentDensity ∂·J = ∂/c∂t(cp)+del·j = ∂p/∂t +del·j = 0 |
| AEM = (ΦEM/c, aEM) | 4-VectorPotential |
||
| QEM
= (EEM/c, pEM) = q AEM = q (ΦEM/c, aEM) |
4-VectorPotentialMomentum | ||
| PEM
= (E/c + qΦEM/c, p +
qaEM)
= γ mo(c,u) PEM = Π = P + qAEM = moU + qAEM =(H/c,pEM) = (γmoc+q ΦEM/c,γmou+q aEM) |
4-MomentumEM 4-CanonicalMomentum 4-TotalMomentum |
||
| D = ∂ + iq/hbar AEM | "The same KG equation, but with
minimal coupling to an EM potential" D·D = = -(moc/hbar)2 (∂ + iq/hbar AEM)·(∂ + iq/hbar AEM) + (moc/hbar)2 = 0 |
Schroedinger Equation (with
external potential) (i hbar)( ∂t ) = V[x] - (hbar)2(del)2/2mo |
E2 = p·p c2 + mo2c4:
Energy of a particle has a Momentum component and a RestMass
component
Total Energy: E = mc2 = γ[u] moc2
= hbarω
Kinetic Energy: T = mc2-moc2
= (γ[u]-1) moc2 = (γ-1) moc2
Rest
Energy: Eo = moc2
|
|___
|
|
| |γ[u]
| m
|
| |
|___|____
mo
Relativistic
(apparent) mass m = AreaLike = γ[u] * mo = hbar
w/c2 = E/c2
Theoretically, this would scale
like a δ-function for photons{mo -->0,u
-->c,γ-->Infinity}
Thus, the relativistic mass of a
photon is proportional to w, the angular frequency
There is also a
rest frequency ωo = moc2/hbar,
even when the massive particle is at rest. Mass is always "spinning"
about the time dimension.
U·U = c2
, d/dτ(U·U) = d/dτ(c2) = 0 ,
d/dτ(U·U) = 2*(U·dU/dτ)
= 2*(U·A) = 0
U·A = 0:
The 4-Acceleration is orthogonal to its own 4-Velocity (Any
acceleration is orthogonal to its own world-line, i.e. you don't
accelerate in time).
U plays the part of the tangent
vector of the world-line, and A plays the part of the normal
vector of the world-line.
The curvature of a world-line is given
by a/c2.
U1·U2
= γ[u1]γ[u2](c2-u1·u2)
= γ[ur]c2 (The scalar product of two
uniformly moving particles is proportional to the γ factor of
their relative velocities)
∂·R =
(∂/c∂t,-del)·(ct,r) =
(∂/c∂t[ct]+del·r) = (∂/∂t[t]+del·r)
= (1+3) = 4
∂·R = 4 The divergence of open
space is equal to the number of independent dimensions
d/dτ
(∂·R) = d/dτ (4) = 0
d/dτ (∂·R)
= d/dτ (∂) · R + ∂·d/dτ (R)
= d/dτ (∂) · R + ∂·U = γ
d/dt (∂) · R + ∂·U = γ
d/dt (∂)·R + ∂·U = γ
(d/dt(∂/c∂t), -d/dt(del))·(ct,r) + ∂·U
= γ (d/dt(∂/c∂t)(ct)+d/dt(del))·r +
∂·U= γ (d/dt(∂/∂t)(t)+d/dt(del))·r
+ ∂·U = γ (d/dt(1)+d/dt(3))+
∂·U = ∂·U
thus,
∂·U
= 0, which is the general SR continuity equation, one might say the
conservation of event flux.
Due to this property, any Lorentz scalar
constant times 4-Velocity U is a conserved quantity.
For
example, let N = noU, so ∂·N
= ∂·noU = no∂·U
= no(0) = 0. The quantity no is
conserved.
Alternately, ∂·U = (∂/c∂t,
-del)·γ(c, u) = ∂·Uo = (∂/c∂t,
-del)·(c, 0) = ∂/c∂t (c) = ∂/∂t (1)
= 0
Compton Scattering
P·P
= (moc)2 ==>0 for photons
Pphot1·Pphot2
= hbar2K1·K2
= (hbar2ω1ω2/c2)(1-n1·n2)
= (hbar2ω1ω2/c2)(1-cos[ų])
Pphot·Pmass
= hbarK·P = (hbarω/c)(1,n)·(E/c,p)
= (hbarω/c)(E/c-n·p) =
(hbarωEo/c2) = (hbarωmo)
Pphot
+ Pmass = P'phot +
P'mass Conservation of 4-Momentum in
Photon-Massive Interaction
Pphot + Pmass
- P'phot = P'mass
rearrange
(Pphot + Pmass
- P'phot)2 = (P'mass)2
square to get scalars
(Pphot·Pphot
+ 2 Pphot·Pmass
- 2 Pphot·P'phot
+ Pmass·Pmass
- 2 Pmass·P'phoot
+ P'phot·P'phot)
= (P'mass)2
(0 + 2 Pphot·Pmass
- 2 Pphot·P'phot
+ (moc)2 - 2 Pmass·P'phot
+ 0) = (moc)2
Pphot·Pmass
- Pmass·P'phot
= Pphot·P'phot
(hbarωmo)-(hbarω'mo)
= (hbar2ωω'/c2)(1-cos[ų])
(ω-ω')/(ωω')
= (hbar/moc2)(1-cos[ų])
(1/ω'-1/ω)
= (hbar/moc2)(1-cos[ų])
ω = 2 pi v = 2 pi c / λ : 1/ω = λ / 2 pi c : hbar = h / 2 pi
(λ'-λ)
= (h/moc)(1-cos[ų])
(λ'-λ) =
(h/moc)(2sin2[ų/2]) Compton scattering
with Compton wavelength (h/moc)
(moc2)(1/E'-1/E)
= (1-cos[ų])
Relativistic
Doppler Effect
A = (ao, a), a
generic SR 4-vector under observation, relative to observer
A·U
= a Lorentz invariant, upon which all observers agree
take A·U
--> A·Uo = (ao,
a)·(c,0) = cao = the
value of the temporal component of A as seen by observer
U
now, let there be an observer Uobs
at rest and an emitter Uemit moving with
respect to Uobs
Uobs
= (c,0): observer at rest
Uemit =
γ(c,v): velocity of emitter relative to
observer
---
A·Uobs = (ao, a)·(c,0) = c ao
= cao_obs
A·Uemit
= (ao, a)·γ(c,v) = γ(cao
- a·v)= cao_emit
---
A·Uobs
/ A·Uemit = cao_obs
/ cao_emit = ao_obs / ao_emit
A·Uobs
/ A·Uemit = cao
/ γ(cao -
a·v) = 1 / γ(1 - a·v/aoc)
= 1 / γ[1 - (|a|/ao)*(n·v/c)]
---
ao_obs
/ ao_emit = 1 / γ(1 - (|a|/ao)*(n·v/c))
ao_obs =
= ao_emit / γ(1 - (|a|/ao)*(n·v/c))
= ao_emit / γ(1 - (|a|/ao)*(n·β))
= ao_emit / γ(1 - (|a|/ao)*(β cos[θ]))
if A is photonic, then (|a|/ao)
= 1, then ao_obs = ao_emit / γ(1 - (n·v/c))
= ao_emit / γ(1 - (n·β))
= ao_emit √[1+|β|]√[1-|β|] / (1 - (n·β))
thus, for photonic Doppler shifts,
if {n toward and β toward obs},
then ao_obs
= ao_emit / γ[1 - |β| Cos[0°]] = ao_emit /
γ[1 - |β|] = ao_emit √[(1+|β|)/(1-|β|)]
-->Doppler BlueShift
---
if {n toward and β 90° to obs},
then ao_obs
= ao_emit / γ[1 - (|β| Cos[90°])] = ao_emit /
γ[1 - 0] = ao_emit /
γ -->the transverse Doppler effect
---
if {n toward and β away from obs},
then ao_obs
= ao_emit / γ[1 - |β| Cos[180°]] = ao_emit /
γ[1 + |β|] = ao_emit √[(1-|β|)/(1+|β|)]
-->Doppler RedShift
Note that ao could be any temporal component,
ie. (E/c) for 4-Momentum P, (ω/c) for 4-Wavevector K,
(ρc) for 4-CurrentDensity J, etc.
Commonly used notation would be the 4-frequency, for which ao
= ν/c,
leading to:
thus, for photonic frequency Doppler shifts,
if {n toward and β toward obs}, then νobs
= νemit √[(1+|β|)/(1-|β|)]
-->Doppler BlueShift
if {n toward and β 90° to obs}, then νobs
= νemit /
γ -->the transverse Doppler effect
if {n toward and β away from obs}, then νobs
= νemit √[(1-|β|)/(1+|β|)]
-->Doppler RedShift
U = γ(c, u), P =
(E/c,p), d(P) = (dE/c,dp)
U·d(P)
= γ(c dE/c-u·dp) = γ(dE-u·dp)
= γ(T dS - P dV + µ dN) = (To dSo
- Po dVo + µo dNo)
= 0 ??
|
U·d(P) = γ(dE-u·dp) = (TodSo - PodVo + µodNo) = const = ? 0 ? |
U·d(P) =
γ(dE-u·dp) = γ(T dS - P dV +
Sum[µi dNi] + w·dL +
E·dP + B·dM) ???
E =
Energy, [Total energy of system]
u = Velocity, p =
Momentum, [Translational/Kinetic energy]
T = Temperature, S =
Entropy [Heat energy]
P = Pressure, V = Volume [Mechanical
compression energy?]
µ = Chemical Potential, N = Particle
Number, ["Chemical" energy = energy per particle] (Sum over
different particle types)
w = Angular Velocity, L =
Angular Momentum, [Rotational energy]
E = Electric Field, P
= Polarization, [Electrical energy]
B = Magnetic Field, M
= Magnetization, [Magnetic energy]
Always have (intensive var *
differential extensive var), intensive = sys size independent,
extensive = sys size proportional
U = γ(c, u),
P = (E/c,p), U·U = c2 ,
P·P = (moc)2
U·P
= γ(c E/c-u·p) = γ(E-u·p)
= γ(T S - P V + µ N) = (To So
- Po Vo + µo No)
?
|
U·P = γ(E-u·p) = (To So - Po Vo + µo No) = moc2 ? for a spatially homogeneous system: relativistic Gibbs-Duhem eqn. |
|
Invariants |
P = Pressure = Po |
N = ParticleNum = No |
S = Entropy = So |
|
Variables |
V = Volume = (1/γ)Volo |
µ = ChemPoten = (1/γ)µo |
T = Temperature = (1/γ)Tempo |
V*P (particle superstructure = Vol*Press)
µ*N
(particle structure = ChemPoten*ParticleNum)
T*S (particle
substructure = Temp*Entropy)
Time t = γ to
Length
L = Lo/γ
Heat Q = q/γ
dq
= TodSo
InertialMassDen(of radiation field)
q = P/vV = γ q
Total Particle Number N = No
is an invariant, because the NumberDensity n varies as n = γ
no, but this is balanced by Volume V = Vo/γ
NumberDenstiy n = γ no where NumberFlux 4-Vector
N = (cn,nf) = no γ(c,
u) = noU,no =
No/(Δ_xo*Δ_yo*Δ_zo)
N
= n * V = (γ no)*(Vo/γ) = no*
Vo = No
N·N =
(noc)2
Total Entropy S = So
is an invariant, because the EntropyDensity s varies as s = γ
so, but this is balanced by Volume V = Vo/γ
EntropyDensity s = γ so where EntropyFlux
4-Vector S = (cs,sf) = so
γ(c, u) = soU,so =
So/(Δ_xo*Δ_yo*Δ_zo)
S
= s * V = (γ so)*(Vo/γ) = so*
Vo = So
S·S = (soc)2
Action S = S(ct,x,y,z)
dS/dτ = 0
dS/dτ = U·∂(S)
= γ(∂S/∂t + u·del(S)) = 0
see
Menzel pg.172
√[1+x] ~ (1+x/2) for
x<<1 This mathematical formula is used to derive the
Newtonian limit
of the various relativistic entities
γ = (1 / √[1-(v/c)2]
)
γ --> 1 for v<<c
All of the formulas below can also be generated from the 4-Velocity
Relation and multiplying by the appropriate Lorentz scalar:
U·U
= γ[u]2(c2-u·u)
= c2
γ2(1-β·β)
= 1
γ2
= 1 + γ2β2
γ
= ±√[1 + γ2β2]
γ ~ ± [1 + γ2β2/2] for (γ2β2
<< 1)
4-Momentum
P = (E/c, p)
P·P = (Eo/c)2 = (moc)2
E2 = Eo2 + p·p c2
E = ±Eo√[ 1 + p·p c2 / Eo2]
E ~ Eo( 1 + p·p c2 / 2 Eo2
+ ...) for | p·p c2 | << | Eo2
| and choosing the positive root and discarding
higher order terms...
E ~ ( Eo + p·p c2 / 2 Eo ) for
| p·p c2 | << | Eo2 |
E ~ ( Eo + p·p / 2 mo ) for | p·p
c2 | << | Eo2 | where Eo
= moc2
E ~ ( Eo + |p|2 /
2 mo ) for | p c | << | Eo
|
Total Energy = Rest Energy + Newtonian Momentum
term
alternately:
γ ~ ± [1 + γ2β2/2]
γEo ~ ± Eo[1 + γ2β2/2]
E ~ ± [Eo + γ2Eoβ2/2]
E ~ ± [Eo + γ2moc2β2/2]
E ~ ± [Eo + γ2mo2c2β2/2mo]
E ~ ± [Eo + γ2mo2v2/2mo]
E ~ ± [Eo + p2/2mo]
4-WaveVector
K = (ω/c, k)
K·K = (ωo/c)2 = (Eo/hbarc)2
=
(moc / hbar)2
ω2 = ωo2 + k·k c2
ω = ±ωo √[ 1 +
k·k c2 / ωo2 ]
ω ~ ωo( 1 + k·k c2 / 2 ωo2
+ ...) for | k·k c2 | << | ωo2
| and choosing the positive root and discarding
higher order terms...
ω ~ ( ωo + k·k c2 / 2 ωo
) for | k·k c2 | << | ωo2
|
ω ~ ( ωo + hbar k·k
/ 2 mo ) for | k·k c2 | << |
ωo2 | where ωo
= moc2 / hbar
ω ~ ( ωo +
hbar |k|2 / 2 mo ) for | k
c | << | ωo
|
Total Angular Frequency = Rest Angular Frequency + Newtonian Wave
Number term
4-Gradient (Wave equation)
∂ = ∂/∂xμ =
(∂/c∂t, -del) =
(∂t/c,
-del)
∂·∂ = (∂to/c)2 =
(- i moc / hbar )2: Klein-Gordon
Relativistic Wave eqn.
∂t2 = ∂to2 + del·del
c2
∂t = ±∂to√[ 1 +
del·del c2 / ∂to2]
∂t ~ ∂to( 1 + del·del c2
/ 2 ∂to2 + ...) for | del·del c2
| << | ∂to2 | and choosing the positive
root and discarding
higher order terms...
∂t ~ (
∂to + del·del c2 / 2
∂to ) for | del·del c2 | <<
|
∂to2 |
∂t ~ (
∂to - hbar del·del / i 2 mo
) for |
del·del c2 | << |
∂to2 | where
∂to
= - i moc2 / hbar
∂t ~ (
∂to - hbar |del|2 / i 2 mo
) for |
del c | << |
∂to
|
or, in more standard form
i hbar ∂t ~ ( i hbar ∂to
- hbar2 |del|2 /
2 mo ) for | del c | << |
∂to
| where i hbar ∂to = Eo, the rest
energy of the potential V
i hbar ∂t ~ ( V(x,t) - hbar2
|del|2 /
2 mo ) for | del c | << |
∂to
|
Time dependent Schroedinger equation is just the Newtonian
approximation of
the Klein-Gordon
Relativistic Wave eqn.
4-ProbabilityCurrentDensity (change in form of Probability Density)
J = (cρ, j) = (ihbarρo/2mo)(ψ*∂[ψ]-∂[ψ*]ψ)
taking the temporal component, the relativistic probability density
ρ = (ihbarρo/2moc2)(ψ* ∂t[ψ]-∂t[ψ*]
ψ)
assume wave solution in following general form:
ψ = A f [k] e(-iωt) and ψ* = A* f [k]* e(+iωt)
then
∂t[ψ] = (-iω)A f [k] e(-iωt)
= (-iω)ψ and ∂t[ψ*] = (+iω)A* f [k]*
e(+iωt) = (+iω)ψ*
then
ρ = (ihbarρo/2moc2)(ψ* ∂t[ψ]-∂t[ψ*]
ψ)
ρ = (ihbarρo/2moc2)((-iω)ψ*ψ-(+iω)ψ*ψ)
ρ = (ihbarρo/2moc2)((-2iω)ψ*ψ)
ρ = (hbarωρo/moc2)(ψ*ψ)
now use the Newtonian form of ω from above
ρ ~ [hbar( ωo +
hbar |k|2 / 2 mo )ρo/moc2](ψ*ψ)
ρ ~ [(hbarωoρo/moc2)
+ (hbarhbarρo |k|2 /
2 momoc2)](ψ*ψ)
ρ ~ ρo[(hbarωo/moc2)
+
(hbarωohbarωo |k|2c2
/ 2 ωoωomoc2moc2
)](ψ*ψ)
ρ ~ ρo[(1) + ( |k|2c2 / 2 ωo2)](ψ*ψ),
but | k c | << | ωo
|
ρ ~ ρo[(1) + (~0)](ψ*ψ) because 2nd term is very
small in non-relativistic limit
ρ ~ ρo(ψ*ψ)
The standard probability density ρo(ψ*ψ) is the Newtonian
approximation of the temporal component of the 4-ProbabilityCurrent,
where ρo is typically set to 1
Alternately, use ω = γωo
ρ = (hbarωρo/moc2)(ψ*ψ)
ρ = (hbarγωoρo/moc2)(ψ*ψ)
ρ = (γρo)(ψ*ψ)
ρ ~ (ρo)(ψ*ψ) where γ->1 in the Newtonian
limit
∂·∂ = (∂/c∂t,-del)·(∂/c∂t,-del)
= ∂2/c2∂t2-del·del
= -(moc / hbar)2: Klein-Gordon
Relativistic Wave eqn.
DEM
= (∂/c∂t + iq/hbar
VEM/c,
-del
+ iq/hbar aEM) =
∂ + (iq/hbar)AEM
DEM·DEM
= -(moc / hbar)2: Klein-Gordon
Relativistic Wave eqn. in electromagnetic potentials
(∂ +
(iq/hbar)AEM)·(∂ +
(iq/hbar)AEM) = -(moc
/ hbar)2: Klein-Gordon Relativistic Wave eqn.
w/ electromagnetic potentials
(∂·∂) +
(iq/hbar)(∂·AEM +
AEM·∂) + (iq/hbar)2(AEM·AEM)
= -(moc / hbar)2: Klein-Gordon
Relativistic Wave eqn. w/ electromagnetic potentials
if (∂·AEM
+ AEM·∂) = 0
then (∂·∂)
+ (iq/hbar)2(AEM·AEM)
= -(moc / hbar)2
(∂/c∂t,-del)·(∂/c∂t,-del)
+ (iq/hbar)2((VEM/c,
aEM)·(VEM/c,
aEM))
= -(moc / hbar)2
(∂2/c2∂t2-del·del)
+ (iq/hbar)2( (VEM/c)2-(aEM·aEM)
) = -(moc /
hbar)2
(∂2/c2∂t2+(iq/chbar)2(VEM2)-(del·del+(iq/hbar)2(aEM·aEM)
) = -(moc / hbar)2
The Klein-Gordon equation is more general than the Schrödinger
equation, but simplifies to the Schrödinger
equation in the (φ/c)<<1 limit.
∂·∂ = (∂/c∂t,-del)·(∂/c∂t,-del) = ∂2/c2∂t2-del·del
= -(moc
/ hbar)2: Klein-Gordon Relativistic Wave eqn.
∂2/c2∂t2 = del·del-(moc
/ hbar)2
∂2/c2∂t2 = (imoc / hbar)2+del·del
(i hbar)2∂2/c2∂t2
= (i hbar)2(imoc / hbar)2+(i
hbar)2del·del
(i hbar)2∂2/c2∂t2
= (moc)2+(i hbar)2del·del
(i hbar)2∂2/∂t2 = (moc2)2*[1
+ (i hbar/moc)2del·del]
(i hbar)∂/∂t = ± (moc2)*Sqrt[1 +
(i hbar/moc)2del·del]
(i hbar)∂/∂t ~ ± (moc2)*[1 +
(1/2)*(i hbar/moc)2del·del
+
...] for ( hbar)2*del·del<<(moc)2
,generally a very good approx. for non-relativistic systems
(i hbar)∂/∂t ~ ± [(moc2) + (i2
hbar2/2mo)del·del + ...]
choosing the positive root and discarding higher order terms...
(i hbar)∂/∂t ~ (moc2) - ( hbar2/2mo)|del|2
(i hbar)∂/∂t ~ - ( hbar2/2mo)|del|2
becomes the time dependent Schrödinger eqn. for a free particle
Also, extensions into EM fields (or other types of relativistic
potentials) can be made using D = ∂ + iq/hbar
AEM
where AEM is the EM vector potential and q is the EM
charge,
and allowing D·D = -(moc/hbar)2
to be the more
correct EM quantum wave equation.
D·D = -(moc/hbar)2
(∂ + iq/hbar AEM)·(∂ + iq/hbar
AEM) + (moc/hbar)2 =
0
let A'EM = iq/hbar AEM
let M = moc/hbar
then (∂ + A'EM)·(∂ + A'EM)
+ (M)2 = 0
∂·∂ + ∂·A'EM + 2 A'EM·∂
+ A'EM·A'EM + (M)2
= 0
now the trick is that factor of 2, it comes about by keeping track of
tensor notation...
a weakness of strick 4-vector notation
let the 4-Vector potential be a conservative field, then ∂·AEM
= 0
(∂·∂) + 2(A'EM·∂) + (A'EM·A'EM)
+ (M)2 = 0
expanding to temporal/spatial components...
( ∂t2/c2-del·del ) + 2(φ'/c ∂t/c - a'·del
) + ( φ'2/c2- a'·a' ) + (M)2 = 0
gathering like components
( ∂t2/c2 + 2φ'/c ∂t/c + φ'2/c2
) - (del·del + 2
a'·del + a'·a' ) + (M)2 = 0
( ∂t2 + 2φ'∂t
+ φ'2 ) - c2(del·del + 2 a'·del +
a'·a'
) + c2(M)2 = 0
( ∂t + φ' )2 - c2(del + a' )2 + c2(M)2
= 0
multiply everything by (i hbar)2
(i hbar)2( ∂t + φ' )2 - c2(i
hbar)2(del + a'
)2 + c2(i hbar)2(M)2
= 0
put into suggestive form
(i hbar)2( ∂t + φ' )2 = - c2(i
hbar)2(M)2 + c2(i hbar)2(del
+ a' )2
(i hbar)2( ∂t + φ' )2
= i2c2(i hbar)2(M)2
+ c2(i hbar)2(del + a' )2
(i hbar)2( ∂t + φ' )2
= i2c2(i hbar)2(M)2
[1 + c2(i hbar)2(del + a' )2/ i2c2(i
hbar)2(M)2 ]
(i hbar)2( ∂t + φ' )2
= i2c2(i hbar)2(M)2
[1 + (del + a' )2/
i2(M)2 ]
take Sqrt of both sides
(i hbar)( ∂t + φ' ) = ic(i hbar)(M)
Sqrt[1 + (del + a' )2/
i2(M)2 ]
use Newtonian approx Sqrt[1+x] ~ ±[1+x/2] for x<<1
(i hbar)( ∂t + φ' ) ~ ic(i hbar)(M)
±[1 + (del + a' )2/2
i2(M)2 ]
(i hbar)( ∂t + φ' ) ~ ±[ic(i hbar)(M)
+ ic(i hbar)(M)(del + a'
)2/2 i2(M)2 ]
(i hbar)( ∂t + φ' ) ~ ±[c(i2 hbar)(M)
+ c( hbar)(del + a'
)2/2(M) ]
remember M = moc/hbar
(i hbar)( ∂t + φ' ) ~ ±[c(i2 hbar)(moc/hbar)
+ c( hbar)(del + a'
)2/2(moc/hbar) ]
(i hbar)( ∂t + φ' ) ~ ±[c(i2)(moc)
+ (hbar)2(del + a'
)2/2(mo) ]
(i hbar)( ∂t + φ' ) ~ ±[-(moc2)
+ (hbar)2(del + a'
)2/(2mo) ]
remember A'EM = iq/hbar AEM
(i hbar)( ∂t + iq/hbarφ ) ~ ±[-(moc2)
+ (hbar)2(del + iq/hbara )2/2mo ]
(i hbar)( ∂t ) + (i hbar)(iq/hbar)(φ)
~ ±[-(moc2) + (hbar)2(del
+ iq/hbara )2/2mo
]
(i hbar)( ∂t ) + (i2)(qφ ) ~
±[-(moc2) + (hbar)2(del
+ iq/hbara )2/2mo
]
(i hbar)( ∂t ) -(qφ ) ~ ±[-(moc2)
+ (hbar)2(del + iq/hbara )2/2mo ]
(i hbar)( ∂t ) ~ (qφ )±[-(moc2)
+ (hbar)2(del + iq/hbara )2/2mo ]
take the negative root
(i hbar)( ∂t ) ~ (qφ ) + [(moc2)
- (hbar)2(del + iq/hbara )2/2mo ]
Here is the general Newtonian result
(i hbar)( ∂t ) ~ (qφ ) + (moc2)
- (hbar)2(del + iq/hbara )2/2mo
or
(i hbar)( ∂t ) ~ (qφ ) + (moc2)
+ [( hbar / i )del + qa
]2/2mo
call (qφ ) + (moc2) = V[x]
(i hbar)( ∂t ) ~ V[x] - (hbar)2(del
+ iq/hbara )2/2mo
typically the vector potential is zero in most non-relativistic settings
(i hbar)( ∂t ) ~ V[x] - (hbar)2(del)2/2mo
And there you have it, the Schrodinger Equation with a potential
The assumptions for non-relativistic equation were:
Conservative field AEM, then ∂·AEM
= 0
(del + a' )2/ i2(M)2
= (del + a' )2/ i2(moc/hbar)2
= (hbar)2(del + a'
)2/ i2(moc)2 is near zero
i.e. (hbar)2(del + a'
)2 << (moc)2, a good
approximation for low-energy systems
Arbitrarily chose vector potential a=0
Or keep it around for a near-Pauli equation (we would just have to
track spins, not included in this derivation)
(K = mo/hbarU = ωo/c2
U) gives (c2/vphase n = u)
Both the wave vector and particle velocity point in the same
direction; along the worldline. The product of the phase velocity and
the particle velocity always equals c2. ( vphase
* u = c2 ). In the case of photons, the phase velocity =
particle velocity = c. In the case of matter particles, the phase
velocity vphase = c2/u > c and particle
velocity u<c. What does this mean? Suppose that you have a
collection of particles traveling at identical velocities that all
flash at the same time. The vphase is the speed at which
the flash moves in other reference frames, and can be considered the
speed of propagation of simultaneity. For particles which are at
rest, the vphase is infinite, which makes sense since they
all appear to flash simultaneously. vphase (the phase
velocity) is sometimes known as the celerity.
(∂·∂)AEM
= µ0 J+∂(∂·AEM)
Inhomogeneous Maxwell Equation
(∂·∂)AEM
= µ0 J Homogeneous Maxwell/Lorentz Equation
(if ∂·AEM = 0 Lorenz
Gauge)
∂·J = ∂ρ/∂t +del·j
= 0 Conservation of EMcurrent
Psi = a E e -iK·R
Photon Wave Equation (Solution to Maxwell Equation)
E·K
= 0 The Polarization of a photon is orthogonal to the WaveVector of
that photon
V·Uobs = γv(c,v)·γ[uobs]
uobs = γvγ[uobs](c2-v·uobs)
V·Uobs[uobs
= 0]/c2 = γv (RestFrame Invariant
expression for
relative gamma factor)
P·Uobs =
E/c γ[uobs]c-p·γ[uobs]
uobs = γ[uobs](E-p·uobs)
P·Uobs[uobs
= 0] = E (RestFrame Invariant expression for energy)
K·Uobs
= w/c γ[uobs]c-k·γ[uobs]
uobs = γ[uobs](w-k·uobs)
K·Uobs[uobs
= 0] = w (RestFrame Invariant expression for angular
frequency)
R·Uobs = ct
γ[uobs]c-r·γ[uobs]
uobs = γ[uobs](c2t-p·uobs)
R·Uobs[uobs
= 0]/c2 = t (RestFrame Invariant expression for
time)
J·Uobs = cp
γ[uobs]c-j·γ[uobs]
uobs = γ[uobs](pc2-j·uobs)
J·Uobs[uobs
= 0]/c2 = ρ (RestFrame Invariant expression
for ElecChargeDensity)
Fuv = ∂uAv-∂vAu
Electromagnetic Field Tensor (F0i = -Ei,Fij
= eijkBk)
L = -1/4 Fuv
Fuv - Ju Au :
Lagrangian Density for EM field
L = -moc2/γ
-V: Relativistic Lagrangian function of a Particle in a Conservative
Potential
VEM = q U·AEM/γ:
Potential of EM field
LEM = -moc2/γ
- q U·AEM/γ = - (P·P/mo
+ qU·AEM)/γ = - (moU·U
+ qU·AEM)/γ
d/dτ
= U·∂ = γ d/dt
U·∂/γ
= ∂/∂t + u·del = d/dt : Convective
Derivative
Larmor formula can be written in Lorentz invariant
form
P = -( q2/ 6πεoc3)(A·A)
= -(μoq2)/(6πc)(A·A) Guassian
units?
=
( q2/ 6πεoc3) γ6/
(u'2 - (u x u')2/c2)
=
( q2/ 6πεoc3) γ6/
(β'2 - (β x
β')2)
=
(2q2/ 3c(1-β'2)3) γ6/
(
β'2 - (
β x
β')2) SI Units?
alternate Larmor formula:
P = (-2/3)(q2/ mo2c3)(F·F)
SI units?
P = -( q2/ 6πεomo2c3)(F·F)
Guassian units?
Relativistic
Power radiated by moving charge by Abraham-Lorentz-Dirac force
P
= (μoq2a2γ6)/(6πc)
Liénard-Wiechert
potentials - potential due to a moving charge
Aμ(x)
= (q/c4πεo) Uμ / ( Rν Uν
) where Rν is a null vector (Rν Rν
= 0)
AEM = (q/c4πεo)
U / (R·U) where (R·R
= 0, the definition of a light signal)
= (q/c4πεo)
U / ( cγ ( |r|-r·u/c ) )
=
(q/c24π εo)(c,u)/(
|r|-r·u/c )
and therefore
φEM
= (q / 4 π εo ) 1/[ r - r·u/c]
aEM = (µ0 q / 4 π)
[u]/[ r - r·u/c]
where terms in square
brackets [] indicate retarded quantities
(R·U)
= (ct,r)·γ(c,u) = γ(c2t -
r·u) = cγ(ct - r·u/c)
tret
= t - |x-x'|/c: (retarded time)
ru
= r - r u/c = the virtual present radius vector;
i.e., the radius vector directed from the position the
charge would occupy at time t' if it had continued with uniform
velocity from its retarded position to the field point.
F
= - grad V(x): Particle moving in conservative force
field
mc2 + V(x) = E = const: Relativistic energy
conservation in conservative force fields
T = mc2-moc2
= (γ[u]-1) moc2 = (γ-1) moc2
Relativistic Kinetic Energy:
F·dX/dt =
dT/dt: Also holds in Relativistic Mechanics
F·U
= (moA+(dmo/dτ)U)·U
= c2(dmo/dτ) = γc2(dmo/dt)
Relativistic Perfect Fluids, where dissipative effects
(viscosity, heat
conduction, etc.) are neglected.
Particle 4-Flow N is a conservative quantity whose balance eqn. is
∂·N = 0
N = (cn, nf)
= no γ(c, u) = n(c, u) = noU
∂·N
= ∂n/∂t +del·(nu) = 0, where n=no
γ
∂·N
= ∂no γ/∂t +del·(no γu) = 0
In non-relativistic limit this becomes ∂no/∂t
+del·( nou) = 0
Tαβ
= ((ne+p)/c2)Uα Uβ - p ηαβ
∂βTαβ
= 0, Consevation of Energy-Momentum Tensor
It can be shown that an scalar (s) and vector (v) which
are related through a continuity equation in all frames of reference
(∂s/∂t + del·v = 0) transform
according to the Lorentz transformations and therefore comprise the
components of a 4-vector V=(cs,v), where ∂ ·V
= 0. Relativistic four-vectors may be identified from the continuity
equations of physics. See A
Proposed Relativistic, Thermodynamic Four-Vector.
Also,
the diffusion equation can be derived from the continuity equation,
which states that a change in density in any part of a system is due
to inflow/outflow of material into/out-of that part of the system.
Essentially, no material is created/destroyed. ∂·J
= ∂p/∂t +del·j = 0
If j is
the flux of diffusing material, then the diffusion equation is
obtained by combining continuity with the assumption that the flux of
diffusing material in any part of the system is proportional to the
local density gradient. j = - D(p) del p.
see
Fick's law of diffusion
Not every vector field has a
scalar potential; those which do are called conservative,
corresponding to the notion of conservative force in physics. Among
velocity fields, any lamellar field has a scalar potential, whereas a
solenoidal field only has a scalar potential in the special case when
it is a Laplacian field.
In vector calculus a conservative
vector field is a vector field which is the gradient of a scalar
potential. There are two closely related concepts: path
independence and irrotational vector fields. Every
conservative vector field has zero curl (and is thus irrotational),
and every conservative vector field has the path independence
property. In fact, these three properties are equivalent in many
'real-world' applications.
An lamellar vector field is a synonym for an irrotational vector field.[1] The adjective "lamellar" derives from the noun "lamella", which means a thin layer. In Latin, lamella is the diminutive of lamina (but do not confuse with laminar flow). The lamellae to which "lamellar flow" refers are the surfaces of constant potential.
An irrotational vector field which is also solenoidal is called a Laplacian vector field.
The fundamental theorem of vector calculus states that any vector
field can be expressed as the sum of a conservative vector field and
a solenoidal field.
In vector calculus a solenoidal vector
field (also known as an incompressible vector field) is a
vector field v with divergence zero:
del·v
= 0
The fundamental theorem of vector calculus states that any vector
field can be expressed as the sum of a conservative vector field and
a solenoidal field. The condition of zero divergence is satisfied
whenever a vector field v has only a vector potential
component, because the definition of the vector potential A
as:
v = del x A
automatically results in the identity (as can be shown, for
example, using Cartesian coordinates):
del·v
= del·(del x A) = 0
The converse also holds: for any solenoidal v there exists a vector potential A such that v = del x A. (Strictly speaking, this holds only subject to certain technical conditions on v, see Helmholtz decomposition.)
In vector calculus, a Laplacian vector field is a vector
field which is both irrotational and incompressible. If the field is
denoted as v, then it is described by the following
differential equations:
del x v = 0
del·v
= 0
Since the curl of v is zero, it follows that v can
be expressed as the gradient of a scalar potential (see irrotational
field) φ:
v = del φ (1)
Then, since the divergence of v is also zero, it follows from equation (1) that
del·del φ = 0
which is equivalent to
del2 φ =
0
Therefore, the potential of a Laplacian field satisfies Laplace's
equation.
In fluid dynamics, a potential flow is a
velocity field which is described as the gradient of a scalar
function: the velocity potential. As a result, a potential flow is
characterized by an irrotational velocity field, which is a valid
approximation for several applications. The irrotationality of a
potential flow is due to the curl of a gradient always being equal to
zero (since the curl of a gradient is equivalent to take the cross
product of two parallel vectors, which is zero).
In case of an incompressible flow the velocity potential satisfies the Laplace's equation. However, potential flows have also been used to describe compressible flows. The potential flow approach occurs in the modeling of both stationary as well as nonstationary flows.
Applications of potential flow are for instance: the outer flow field for aerofoils, water waves, and groundwater flow.
For flows (or parts thereof) with strong vorticity effects, the potential flow approximation is not applicable.
A velocity potential is used in fluid dynamics, when a
fluid occupies a simply-connected region and is irrotational. In such
a case,
del x u = 0
where u denotes the flow velocity of the fluid. As a
result, u can be represented as the gradient of a scalar
function Φ:
u = del Φ
Φ is known as a velocity potential for u.
A velocity potential is not unique. If a is a constant then Φ + a is also a velocity potential for u. Conversely, if Ψ is a velocity potential for u then Ψ = Φ + b for some constant b. In other words, velocity potentials are unique up to a constant.
Unlike a stream function, a velocity potential can exist in three-dimensional flow.
see Cosmological Physics
Relativistic Euler Equations:
dv/dt
= - 1/[γ2(ρ + p/c2)](del p +
p'v/c2): Conservation of Momentum
d/dt[γ2(ρ
+ p/c2)] = p'/c2 - γ2(ρ +
p/c2)del·v: Conservation of
Energy
where p' = ∂ p/∂ t
∂·J = 0
where J = noU (J is the Number Flux
here)
Relativistic Enthalpy w = (ρ + p/c2)
d/dt[γw/n]
= p'/γnc2
Thus, in steady flow, γ *
(enthalpy/particle) = const.
In non-relativistic limit these
reduce to
dv/dt = - 1/[ρ](del p): Conservation
of Momentum
d/dt[(ρ)] = - (ρ)del·v:
Conservation of Mass
p = Pressure
ΔE = - p ΔV
E
= ρ c2 V
ΔV / V = - Δρo/ρo
Relativisitic
Bernoulli's eqn.
γ w / ρo = const
Equation of motion for a free
particle
d2R/dτ2 = A =
0
Klein-Gordon Relativistic Wave eqn. = Wave
equation for a scalar field (no spins)
(∂·∂)ψ
+ (moc / hbar)2ψ = 0
Maxwell
Equations:
(∂·∂)AEM = µ0
J+∂(∂·AEM)
Inhomogeneous Maxwell Equation
(∂·∂)AEM
= µ0 J Homogeneous Maxwell/Lorentz Equation
(if ∂·AEM = 0 Lorenz
Gauge)
where AEM = µ0
Integral[ [ J ]/r dV] ??? is a solution to the Maxwell
Equation
Lorentz Force - Covariant eqn. of motion for a
particle in an EM field:
dPμ / dτ = (q/c) Fμν
dXν / dτ
QED Lagrangian density
L = ψ (i hbar c γμ Dμ - moc2)ψ - (1/4)FμνFμν
plugging into Euler-Lagrange equation gives:
(i hbar c γμ Dμ - moc2) = 0, the Dirac equation in the EM field
and
∂νFνμ = -ecψ γμ ψ = -ejμ, the Maxwell eqations with a source which is the 4-current coming from the Dirac eqn.
| L = -(PT·U)/γ = -moc2/γ - qΦ + qa·u | H = γ(PT·U) = γmoc2 + qΦ = γmoc2 + qγΦo = γ(moc2 + qΦo) | H + L = pT·u |
|
L = -(PT·U)/γ L = -((P + Q)·U)/γ L = -(P·U + Q·U)/γ L = -P·U/γ - Q·U/γ L = -moU·U/γ - qA·U/γ L = -moc2/γ - qA·U/γ L = -moc2/γ - q(Φ/c, a)·γ(c, u)/γ L = -moc2/γ - q(Φ/c, a)·(c, u) L = -moc2/γ - q(Φ - a·u) L = -moc2/γ - qΦ + qa·u L = -moc2/γ - qΦo/γ L = -(moc2 + qΦo)/γ |
H = γ(PT·U) H = γ((P + Q)·U) H = γ(P·U + Q·U) H = γP·U + γQ·U H = γmoU·U + γqA·U H = γmoc2 + qγΦo H = γmoc2 + qΦ assuming A = (Φo/c2) U H = ( γβ2 + 1/γ )moc2 + qΦ H = ( γmoβ2c2 + moc2/γ ) + qΦ H = ( γmov2 + moc2/γ ) + qΦ H = p·u + moc2/γ + qΦ H = E + qΦ H = ±c√[mo2c2+p2] + qΦ H = ±c√[mo2c2+(pT-qa)2] + qΦ |
H + L = γ(PT·U) - (PT·U)/γ (γ - 1/γ)(PT·U) ( γβ2 )(PT·U) ( γβ2 )(moc2 + qΦo) (γmoβ2c2 + qγΦoβ2) (γmou·uc2/c2 + qΦoγu·u/c2) (γmou·u + qa·u) assuming A = (Φo/c2) U (p·u + qa·u) pT·u |
[ ∂u , Rv ]
= ∂u Rv - Rv ∂u
= gμν quantum commutator with pure 4-gradient [since
( Rv ∂u = 0) generally???]
but K = i
d
[ Ku , Rv ] = i gμν
quantum commutator with 4-wave vector
but P = hbar
K
[ Pu , Rv ] = i hbar gμν
quantum commutator with 4-momentum
[ Ru , Pv
] = Ru Pv - Pv Ru = (- i
hbar gμν) SR quantum commutator with
4-momentum
this gives
[ x , px ] = [ y , py
] = [ z , pz ] = (i hbar)
[ ct , E/c ] = [ t
, E ] = (- i hbar) :assuming that one can treat the time
as an operator...
both of these yield the familiar uncertainty
relations:
Generalized Uncertainty relation: (Δ A) * (Δ
B) > = (1/2) |< i[A,B] >| see Sudbury pg. 59 for a great
derivation
(Δ x * Δ px > = hbar
/ 2) and (Δ t * Δ E > = hbar / 2)
or
more generally
(Δ Ru * Δ Pv >
= hbar duv / 2)
or
(Δ Ru
* Δ Kv > = duv / 2)
(Δ x * Δ
kx > = 1/2) and (Δ t * Δ w > = 1/2)
[
Ru , Rv ] = Ru Rv - Rv
Ru = 0 : All position coordinates commute
[ Pu
, Pv ] = Pu Pv - Pv Pu
= 0 : All momentum coordinates commute
While I'm at it, a
small comment about the quantum uncertainty relation. A great many
books state that the quantum uncertainty relations mean that a
"particle" cannot simultaneously have precise properties of
position and momentum. I disagree with that interpretation. The
uncertainty relations, the mathematical structure of the argument,
say nothing about "simultaneous" measurements. They do say
something about "sequential" measurements. A measurement of
one variable places the system in a state such that if the next
measurement is that of a non-commuting variable of the first, then
the uncertainty must be of a minimum>0 amount. Also, note that the
uncertainty relations are not necessarily about the size of h. Nor
are they about the factor of ( i ) in the commutation relation. It
would
appear that they are about the metric gμν itself,
which has a non-zero result for sequential, non-commuting
measurements.
Also, a comment on the EPR results. Based on SR,
one cannot say that the measurement of one particle immediately
"collapses" the physical state of the other. Since the two
entangled particles can be setup such that they are space-like
separated at the "events" of their respective measurement,
there exist coordinate frames in which the measurement of the 1st
particle occurs before that of the 2nd, exactly at the same time as
the 2nd, and after that of the 2nd. Thus, how is the first particle
to "know" that it must collapse the wavefunction of the
2nd, or that it must itself be collapsed by the 2nd?
--------
need
to derive:
(Δ phix * Δ Lx > =
hbar / 2)
where phix is angle about x, and
Lx is angular momentum about x
| time-like
interval(+)
/ light-like interval(0)
worldline
|
| c
\
future /
\ | /
\ | /
-- space-like interval(-)
\|/now
/|\
/
| \
elsewhere
/ | \
/
past \
|
-c
(0,0) Zero-Null Vector
(+a,0)
Future Pointing Pure TimeLike
(-a,0) Past Pointing Pure
TimeLike
(0,b) Pure SpaceLike
(a,b)
|a|>|b| TimeLike
(a,b) |a| =|b|
Photonic-LightLike
(a,b) |a|<|b| SpaceLike
Any TimeLike 4-Vector (a,b) may be boosted into a Pure TimeLike
(ka,0)
state
Any SpaceLike 4-Vector (a,b) may be boosted into a Pure
SpaceLike (0,kb)
state
So far, Poincare Invariance appears to
be an absolute conservation law of all quantum field theories, as
well as being a basis for Special Relativity. A number of quantum
field theories are based on the complex (charged) scalar
(Klein-Gordon) quantum field - which is mathematically the simplest
QFT that still contains a continuous global [U(1)] internal symmetry.
A real (Hermetian) scalar QFT is mathematically still simpler, but
the absence of "charge" renders it uninteresting for most
purposes.
Poincare group (aka inhomogeneous Lorentz group) and
its representations
The set of Lorentz transforms and spacetime
translations (Λ,A) such that:
X'μ = Λμν
Xν + Aμ
with conditions:
Det[Λ]
= +1 (excludes discrete transforms of space inversion =>
proper)
Λ00 >= +1 (excluded
discrete transforms of time inversion => orthochronous, preserve
direction of time)
Λμν (a
Lorentz Transform - maps spacetime onto itself and therefore
preserves the inner product)
Λμν
Λμλ = gνλ (the
Minkowski Metric)
Aμ = (Space-time
Translation)
Unitary Operators representing these
transforms:
U(A,1) = Exp[ i P·A
]
U(0,Λ) = Exp[ i Mμν Λμν
]
Poincare group has 10 generators (spacetime 4-generators)
Pμ
(4 generators of space-time translation = Conservation of
4-Momentum)
Mμν (6 generators of Lorentz group =
3 orbital angular momenta + 3 Lorentz boosts)
[ Pμ,
Pν ] = 0 (Energy/Momentum commutes with itself)
[
Mμν, Pσ ] = - i ( Pμ
gνσ - Pν gμσ
)
or
[ Mμν, Pσ ] = i ( gνσ
Pμ - gμσ Pν ) {one of
these has a sign error I think}
[ Mμν, Mρσ
] = -i ( Mνσ gμρ - Mμσ
gνρ + Mρν gμσ
- Mρμ gνσ )
Then, define
the spatial 3-generators:
"Spatial Rotation" generators
Ji = -(1/2) εijk Mjk (for
i=1,2,3), are Hermetian, (Mjk)† = Mjk
"Lorentz Boost" generators Ki = Mi0
(for i=1,2,3), are anti-Hermetian, (Mi0)†
= - Mi0
[ Ji , Pk ] = i εikl
Pl
[ Ji , P0 ] = 0 (Spin
commutes Energy)
[ Ki , Pk ] = i P0
gik
[ Ki , P0 ] = - i Pi
[
Jm , Jn ] = i εmnk Jk
[
Jm , Kn ] = i εmnk Kk
[
Km , Kn ] = - i εmnk
Jk
Covariance of physical laws under Poincare
trans. imply that all quantities defined in Minkowski space-time must
belong to a representation of the Poincare group. By def., the states
that describe elementary particles belong to irreducible
representations of the Poincare group. These representations can be
classified by the eigenvalues of the Casimir operators, which are the
functions of the generators that commute with all the generators.
This property implies that the eigenvalues of the Casimir operators
remain invariant under group transforms.
Poincare Algebra
ISO(1,3)
There are two Casimir operators of the Poincare group.
They lead, respectively, to mass and spin. Thus, mass and spin are
inevitable properties of particles in a universe where SR is
valid.
(1) P2 = ημν Pμ
Pν = Pμ Pμ with
corresponding eigenvalues P2 = m2
which
measure the invariant mass of field configurations.
In the real
world we observe only time-like or light-like four-momenta, i.e.
particles with positive or zero mass. Furthermore, the temporal
components are always positive.
With dimensional units this would
be P2 = m2c2
(2) W2
= ημν Wμ Wν = Wμ
Wμ with corresponding eigenvalues W2 = ( w02
- w·w ) = - (w·w) = -
(P02j2) = - m2
s(s+1),
which measure the invariant spin of the particle, where
there are (2s+1) spin states
(or 2 polarization/helicity states
for massless fields)
with Wμ as the Pauli-Lubanski
(mixed) Spin-Momentum four vector
With dimensional units this
would be W2 = - m2c2hbar2
s(s+1)
Note: Massless representation give P2 = m2
= 0 and W2 = - m2 s(s+1) = 0
For instance,
for a photonic Pμ = E(1,0,0,1), one has Wμ
= M12 Pμ
so that M12 takes the
possible eigenvalues ± s
Wσ =
(1/2) εσμνρ Mμν
Pρ
or
Wσ = - (1/2) εμνρσ
Mμν Pρ
such that
[ Wσ
, Pμ ] = 0
[ Mμν , Wσ
] = -i ( Wμ gνσ - Wν
gμσ )
[ Wλ , Wσ
] = i ελσαβ Wα
Pβ
Further,
W = (w0,w)
= (p·j , P0j - p x k)
w0 = p·j
w = P0j
- p x k
where
j = (M32,M13,M21)
are the 3 components of angular momentum, where [J1,J2]
= i J3 and cyclic permutations
k = (M01,M02,M03)
are boosts in 3 Cartesian directions
Wigner's classification: (non-negative energy irreducible unitary
representations of the Poincare group)
The irreducible unitary
representations of the Poincare' group are classified according to
the eigenvalues of P2 and W2
They fall into
several classes:
1a) P2 = m2 > 0 and
P0 > 0: Massive particle
1b) P2 = m2
> 0 and P0 < 0: Massive anti-particle??
2a) P2
= 0 and P0 > 0: Photonic
2b) P2 = 0 and
P0 < 0: Photonic??
3) P2 = 0 and P0
= 0: P in the 4-Zero, the vacuum
4) P2 = m2
< 0: Tachyonic
A complete set of commuting observables is
composed of P2, the 3 components of p, W2,
and one of the 4 components of Wμ
The
eigenvalues of P2 (mass) and W2 (spin)
distinguish (possibly together with other quantum numbers) different
particles. This is the general result for finite-mass quantum fields
that are invariant under the Poincare transformation.
In the
case of the scalar field, it is straightforward to identify the
particle content of its Hilbert space.
A 1-particle state |k>
= at(k)|0> is characterized by the
eigenvalues
p0|k> = hbarω(k)|k>,
p|k> = hbark|k>, W2|k>
= 0
thus showing that the quanta of such a quantum field may be
identified with particles of definite energy-momentum and mass m,
carrying a vanishing spin (in the massive case) or helicity (in the
massless case). Relativistic QFT's are thus the natural
framework in which to describe all the relativistic quantum
properties, including the processes of their annihilation and
creation in interactions, or relativistic point-particles. It is the
Poincare invariance properties, the relativistic covariance of such
systems, that also justifies, on account of Noether's theorem, this
physical interpretation.
One has to learn how to extend the above
description to more general field theories whose quanta are particles
of nonvanishing spin or helicity. One then has to consider
collections of fields whose components also mix under Lorentz
transforms.
One may list the representations which are
invariant under parity and correspond to the lowest spin/helicity
content possible.
|
(0,0) |
φ |
scalar field |
|
(1/2,0) (+) (0,1/2) |
ψ |
Dirac spinor |
|
(1/2,1/2) |
Aμ |
vector field |
|
(1,0) (+) (0,1) |
Fuv = ∂uAv-∂vAu |
EM field tensor |
Consider an arbitrary spacetime vector xμ
Construct
the 2 x 2 Hermitian matrix X = X†
|
X = xμσμ = |
( x0 + x3 |
x1 - i x2 ) |
|||||
|
( x1 + i x2 |
x0 - x3 ) |
then Det[X] = x2 = x·x = ημν
xμ xν
see Proceedings
of the Third International Workshop on Contemporary Problems in
Physics, By Jan Govaerts, M. Norbert Hounkonnou, Alfred Z.
Msezane
see Conceptual Foundations of Modern Particle Physics,
Robert Eugene Marshak
see Fundamentals of Neutrino Physics and
Astrophysics, Carlo Giunti
see Kinematical Theory of Spinning
Particles, Martin Rivas
|
Spin |
Statistics |
Relativistic Eqn. |
Relativistic Eqn. |
Field |
Polarizations |
Non-Relativistic Eqn. Newtonian Limit √[1+x] ~ (1+x/2) for x<<1 v<<c |
|
0 |
Boson: |
FreeWave |
Klein-Gordon (-Fock) |
Ψ |
2? |
Schrödinger |
|
1/2 |
Fermion |
Weyl |
Dirac |
Ψ |
2 |
Pauli, (Schrödinger-Pauli) |
|
1 |
Boson |
Maxwell |
Proca |
A |
2 (= 2 transverse) |
|
|
3/2 |
Fermion |
Gravitino? |
Rarita-Schwinger |
ψμ |
2 |
|
|
2 |
Boson |
Einstein |
? ? |
tensor = 2-tensor |
2 |
Duffin-Kemmer-Petiau Equation = Complex Proca Equation
Duffin-Kemmer Equation: ( βμ pμ - M ) ψ = 0
: for a free spin-0 or spin-1 particle
|
Dim |
Type |
|
Hodge Dual |
|
0 |
scalar |
|
|
|
1 |
vector |
|
|
|
2 |
tensor |
|
|
|
3 |
pseudovector |
magnietic field, spin, torque, vorticity, angular momentum |
|
|
4 |
pseudoscalar |
magnetic charge, magnetic flux, helicity |
|
In Minkowski space (4-dimensions), the { 1 4 6 4 1} Hodge dual of
an n-rank (n<=2) tensor will be an (4-n) rank skew-symmetric
pseudotensor
Hodge duals
*dt = dx ^ dy ^ dz
*dx = dt ^ dy ^
dz
*dy = - dt ^ dx ^ dz
*dz = dt ^ dx ^ dy
*(dt ^ dx) =
-dy ^ dz
*(dt ^ dy) = dx ^ dz
*(dt ^ dz) = -dx ^ dy
*(dx ^
dy) = dt ^ dz
*(dx ^ dz) = -dt ^ dy
*(dy ^ dz) = dt ^ dx
Einstein made as stronger statement about EP, known as EPP: In small
enough regions of spacetime, the laws of physics reduce to those of
special relativity; it is impossible to detect the existence of a
gravitational field by means of local experiments.
SR --> QM, what assumptions necessary & where does it break
down
Relational QM
General Continuity of WorldLines
Spin vs.
Accel, time component correlation
Relativistic Thermodynamics &
SM
Poincare Group & Casimir operators & Casimir Invariants
(mass & spin of Poincare field)
Generalized Uncertainty
Points
- Waves - Potentials - Fields
Relation between single point and
density 4-vectors
Poisson Eqn. / Laplace Eqn.
Continuity eqn
--> 4-Vector
Adding Spin to Klein-Gordon
Relativistic
Lagrangian & Hamiltonian
Covariant Form Relativistic
Equations
Umov-Poynting examples
Dirac - Kemmer generalized
eqn.
Hodge Dual examples
Pressure Diffusion Wave/Eqn.
Potential
Flow Theory
Schroedinger Eqn as a diffusion equation
Main article: Schrödinger equation
With a simple division, the Schrödinger equation for a single particle of mass m in the absence of any applied force field can be rewritten in the following way:
This equation is formally similar to the particle diffusion equation, which one obtains through the following transformation:
Applying this transformation to the expressions of the Green functions determined in the case of particle diffusion yields the Green functions of the Schrödinger equation, which in turn can be used to obtain the wavefunction at any time through an integral on the wavefunction at t=0:
Remark: this analogy between quantum mechanics and diffusion is a purely formal one. Physically, the evolution of the wavefunction satisfying Schrödinger's equation might have an origin other than diffusion.
Some examples of equivalent electrical and hydraulic equations:
|
type |
hydraulic |
electric |
thermal |
|---|---|---|---|
|
quantity |
volume V [m3] |
charge q [C] |
heatQ [J] |
|
potential |
pressure p [Pa=J/m3] |
potential φ [V=J/C] |
temperature T [K=J/kB] |
|
flux |
current ΦV [m3/s] |
current I [A=C/s] |
heat transfer rate [J/s] |
|
flux density |
velocity v [m/s] |
j [C/(m2·s) = A/m²] |
heat flux [W/m2] |
|
linear model |
Poiseuille's law |
Ohm's law |
Fourier's law |
Classical Dynamics of Particles & Systems, 3rd Ed.,
Jerry B. Marion & Stephen T. Thornton (Chap14)
Classical
Electrodynamics, 2nd Ed., J.D. Jackson (Chap11,12)
Classical
Mechanics, 2nd Ed., Herbert Goldstein (Chap7,12)
Electromagnetic
Field, The, Albert Shadowitz (Chap13-15)
First Course in
General Relativity, A, Bernard F. Schutz (Chap1-4)
Fundamental
Formulas of Physics, by Donald Howard Menzel
(Chap6)
Introduction to Electrodynamics, 2nd Ed., David J.
Griffiths (Chap10)
Introduction to Modern Optics, 2nd Ed.,
Grant R. Fowles (var)
Introduction to Special Relativity, 2nd
Ed., Wolfgang Rindler (All) (**pg60-65,82-86**)
Lectures on
Quantum Mechanics, Gordon Baym (Chap22,23)
Modern
Elementary Particle Physics: The Fundamental Particles and Forces?,
Gordon Kane (Chap2+)
Path Integrals and Quantum Processes,
Mark Swanson (var)
Quantum Electrodynamics, Richard P.
Feynman (Lec7-rest)
Quantum Mechanics, Albert Messiah
(Chap20)
Quantum Mechanics and the Particles of Nature: An
Outline for Mathematicians, Anthony Sudbery (Chap7)
Spacetime
and Geometry: An Introduction to General Relativity, Sean M.
Carroll (var)
Statistical
Mechanics, by R. K. Pathria
(Chap6.5)
Theory of Spinors, The, E'lie Cartan (var)
Topics
in Advanced Quantum Mechanics, Barry R. Holstein
(Chap3,6,7)
Relativistic
Quantum Fields, Mark Hindmarsh, Sussex, UK
Relativity
and electromagnetism, Richard Fitzpatrick, Associate
Professor of Physics, The University of Texas at
Austin
http://farside.ph.utexas.edu/teaching/em/lectures/node106.html
The
Relativistic Boltzmann Equation: Theory and
Applications, Carlo Cercignani, Gilberto Medeiros
Kremer
Essential
Relativity: Special, General, and Cosmological, by
Wolfgang Rindler
Compendium
of Theoretical Physics, by Armin Wachter, Henning
Hoeber
Relativistic
Quantum Mechanics of Leptons and Fields, by Walter
T. Grandy
This
remains a work in progress.
Please, send
comments/corrections to John