ph300 modern physics sp11
DESCRIPTION
PH300 Modern Physics SP11. “The only reason for time is so that everything doesn’t happen at once.” - Albert Einstein. 2/1 Day 6: Questions? Spacetime Addition of Velocities Lorentz Transformations. Thursday: Relativistic Momentum & Energy. Last time : - PowerPoint PPT PresentationTRANSCRIPT
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PH300 Modern Physics SP11
2/1 Day 6: Questions?SpacetimeAddition of VelocitiesLorentz Transformations
Thursday: Relativistic Momentum & Energy
“The only reason for time is so that everything doesn’t happen at once.”- Albert Einstein
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Today:• Spacetime• Addition of velocities• Lorentz transformations
Next week:Intro to quantumExam I (in class)
Thursday: • Relativistic momentum and energy
HW03 due, beginning of class; HW04 assigned
Last time:• Time dilation and length contraction
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Spacetime Diagrams (1D in space)
In PHYS I:
x
v
t
xΔx
Δtv = Δx/Δt
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Spacetime Diagrams (1D in space)
In PH300:
t
x
x
tc ·
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Spacetime Diagrams (1D in space)
In PH300:
x
tc· object moving with 0<v<c.‘Worldline’ of the object
x
c·t
-2 -1 0 1 2
object at restat x=1
-2 -1 0 1 2
x
c·t
-2 -1 0 1 2
object moving with v = -c.x=0 at time t=0
object moving with 0>v>-c
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Lucy
L R
Ricky
Recall: Lucy plays with a fire cracker in the train.Ricky watches the scene from the track.
v
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Example: Lucy in the train
L Rx
ct
In Lucy’s frame: Walls are at rest
Light travels to both walls
Light reaches both walls at the same time.
Lucy concludes:Light reaches both sides at the same time
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Example: Ricky on the tracks
L Rx
ct
In Ricky’s frame: Walls are in motion
Ricky concludes:Light reaches left side first.
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v=0.5c... -3 -2 -1 0 1 2 3 ...
... -3 -2 -1 0 1 2 3 ...
S
S’
Frame S’ is moving to the right at v = 0.5c. The origins of S and S’ coincide at t=t’=0. Which shows the world line of the origin of S’ as viewed in S?
ct
x
ct
x
ct
x
ct
x
A B C D
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Frame S’ as viewed from S
x
ct ct’This is the time axis of the frame S’
x’
This is the space axis of the frame S’
These angles are equal
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Frame S’ as viewed from S
x
ct ct’
x’
Both frames are adequate for describing events – but will give different spacetime coordinates for these events, in general.
In S: (x=3,ct=3)In S’: (x’=1.8,ct’=2)
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Spacetime Interval
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Distance in Galilean Relativity
mmmm 525)4()3( 22
The distance between the blue and the red ball is:
If the two balls are not moving relative to each other, we find that the distance between them is “invariant” under Galileo transformations.
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Remember Lucy?
Lucyh
Event 1 – firecracker explodesEvent 2 – light reaches detectorDistance between events is h
tch
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Remember Ricky?
Event 1 – firecracker explodesEvent 2 – light reaches detectorDistance between events is cΔt’But distance between x-coordinates is Δx’and: (cΔt’)2 = (Δx’)2 + h2
We can write
hcΔt’
Δx’
xtch 222
And Lucy got
since xtch 222
0x
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Spacetime intervalSay we have two events: (x1,y1,z1,t1) and (x2,y2,z2,t2). Define the spacetime interval (sort of the "distance") between two events as:
The spacetime interval has the same value in all reference frames! I.e. Δs2 is “invariant” under Lorentz transformations.
22222 zyxtcs
x = x2 − x1
Δy = y2 − y1
Δz = z2 − z1
Δt = t2 − t1
With:Spacetime interval
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s '( )2 = cΔt '( )2 − Δx '( )2 − Δy '( )2 − Δz '( )2
Spacetime interval
The spacetime interval has the same value in all reference frames! I.e. Δs2 is “invariant” under Lorentz transformations.
22222 zyxtcs
s '( )2 = Δs( )2
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Spacetime
x
ctHere is an event in spacetime.
Any light signal that passes through this event has the dashed world lines. These identify the ‘light cone’ of this event.
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Spacetime
x
ctHere is an event in spacetime.
The blue area is the future on this event.
The pink is its past.
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Spacetime
x
ctHere is an event in
spacetime.
The yellow area is the “elsewhere” of the event. No physical signal can travel from the event to its elsewhere!
A
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Spacetime
x
ct
A
B
Now we have two events A and B as shown on the left.
The space-time interval (Δs)2 of these two events is:
A) PositiveB) NegativeC) Zero
If (Δs)2 is negative in one frame of reference it is also negative in any other inertial frame! ((Δs)2 is invariant under Lorentz transformation). Causality is fulfilled in SR.
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Spacetime
x
ct
A
B
(Δs)2 >0: Time-like events (A D)
CD
(Δs)2 is invariant under Lorentz transformations.
(Δs)2 <0: Space-like events (A B)
(Δs)2 =0: Light-like events (A C)
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Example: Wavefront of a flash
x
y
z
t=0 t>0
(ct)2 - x2 - y2 - z2 = 0
Wavefront = Surface of a sphere with radius ct:
Spacetime interval for light-like event: (Δs)2 = 0
Einstein: 'c' is the same in all inertial systems.Therefore: (ct')2 - x'2 - y'2 - z'2 = 0 in all inertial systems!(Here we assumed that the origins of S and S' overlapped at t=0)
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Velocity transformation (1D)
... -3 -2 -1 0 1 2...
S
AB
An object moves from event A=(x1,t1) to event B =(x2,t2).
As seen from S, its speed is
As seen from S’, its speed is
txu
txu
Δx
x1x2
... -3 -2 -1 0 1 2 3 ...
S’ v
with: Δx = x2 – x1
Δt = t2 – t1
with: Δx’ = x’2 – x’1
Δt’ = t’2 – t’1
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Velocity transformation (1D)
t
txcvt
tvxtxu
1
1
))/(()(
2
2/1 cuvvuu
Galilean result
New in special relativity
txu
txu
, , where Δx=x2 – x1, Δx’=x’2 – x’1
Use Lorentz: x’ = (x-vt)...
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Velocity transformation in 3D
S
x
z
y
S' x'
z'
y'
v(x,y,z,t)
(x',y',z',t')
u
In a more general case we want to transform a velocity u (measured in frame S) to u’ in frame S’. Note that u can point in any arbitrary direction, but v still points along the x-axes.
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Velocity transformation (3D)
The velocity u=(ux, uy, uz) measured in S is given by:
ux=Δx/Δt , uy=Δy/Δt , uz=Δz/Δt , where Δx=x2-x1 …
To find the corresponding velocity components u’x, u’y, u’z in the frame S’, which is moving along the x-axes in S with the velocity v, we use again the Lorentz transformation:
x’1=γ(x1-vt1), and so on…t’1=γ(t1-vx1/c2), and so on…
Algebra
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Velocity transformation (3D)(aka. “Velocity-Addition formula”)
2/1'
cvuvuu
x
xx
2/1'
cvuu
ux
yy
2/1'
cvuuu
x
zz
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Some applications
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Suppose a spacecraft travels at speed v=0.5c relative to the Earth. It launches a missile at speed 0.5c relative to the spacecraft in its direction of motion. How fast is the missile moving relative to Earth? (Hint: Remember which coordinates are the primed ones. And: Does your answer make sense?)
a) 0.8 c b) 0.5 c c) c d) 0.25 c e) 0
2/1 cuvvuu
2/1 cvuvuu
2
2
/1'
)(
)(
cuvvuu
xcvtt
vtxx
Relativistic transformations
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Velocity transformation: Which coordinates are primed?
Sx
z
y
S' x'
z'
y'
v(x,y,z,t)
(x',y',z',t')
u
SpacecraftEarth
u is what we were looking for!(i.e. velocity measured in S)
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The “object” could be light, too!Suppose a spacecraft travels at speed v=0.5c relative to
the Earth. It shoots a beam of light out in its direction of motion. How fast is the light moving relative to the Earth? (Get your answer using the formula).
a) 1.5c b) 1.25c c) c d) 0.75c e) 0.5c
2/1 cuvvuu
2/1 cvuvuu
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TransformationsIf S’ is moving with speed v in the positive x direction relative to S, and the origin of S and S' overlap at t=0, then the coordinates of the same event in the two frames are related by:
)(
)(
2 xcvtt
zzyy
vtxx
Lorentz transformation(relativistic)
2/1'
cvuvuu
x
xx
2/1'
cvuu
ux
yy
2/1'
cvuuu
x
zz
Velocity transformation(relativistic)
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A note of caution:The way the Lorentz and Galileo transformations are presented here assumes the following:
An observer in S would like to express an event (x,y,z,t) (in his frame S) with the coordinates of the frame S', i.e. he wants to find the corresponding event (x',y',z',t') in S'. The frame S' is moving along the x-axes of the frame S with the velocity v (measured relative to S) and we assume that the origins of both frames overlap at the time t=0.
S
x
z
y
S' x'
z'
y'
v
(x,y,z,t)
(x',y',z',t')
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Application: Lorentz transformation
A Bt0 = 0
v
…
Two clocks (one at A and one at B) are synchronized. A third clock flies past A at a velocity v. The moment it passes A all three clocks show the same time t0 = 0 (viewed by observers in A and B. See left image.)
What time does the third clock show (as seen by an observer at B) at the moment it passes the clock in B? The clock at B is showing t1 = 1s at that moment. Use Lorentz transformation!
A B
v
t1 = 1s
?
)''(
)(
2
2
xcvtt
xcvtt
A) γ · (t1-t0) B) γ2(t1-t0)(1 – v/c2) C) γ2 (t1-t0)(1 + v2/c2)D) (t1-t0) / γ E) γ(t1-t0)(1 + vx'/c2)
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Hint: Use the following frames:
A Bt0 = 0
…A B
v
t1 = 1s
?
)''(
)(
2
2
xcvtt
xcvtt
v
x'x
The moving clock shows the proper time interval!! Δtproper = Δt / γ
Two clocks (one at A and one at B) are synchronized. A third clock flies past A at a velocity v. The moment it passes A all three clocks show the same time t0 = 0 (viewed by observers in A and B. See left image.)
What time does the third clock show (as seen by an observer at B) at the moment it passes the clock in B? The clock at B is showing t1 = 1s at that moment. Use Lorentz transformation!A) γ · (t1-t0) B) γ2(t1-t0)(1 – v/c2) C) γ2 (t1-t0)(1 + v2/c2)D) (t1-t0) / γ E) γ(t1-t0)(1 + vx'/c2)
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Hint: Use the following systems:
A Bt0 = 0
…A B
v
t1 = 1s
?
)( 2 xcvtt
vx'x
The clock travels from A to B with speed v. Assume A is at position x = 0, then B is at position x = v·t, t=(t1-t0)
Use this to substitute x in the Lorentz transformation:
t = γ (t −v2tc2 ) = γ t(1 −
v2
c2 ) = t / γ
We get exactly the expression of the time dilation!
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Relativistic mechanics
Previously:Ideas of space and time
Next:Ideas of momentum and energy
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MomentumThe classical definition of the momentum p of a particle with mass m is: p=mu.
In absence of external forces the total momentum is conserved (Law of conservation of momentum):
.1
constn
ii
p
Due to the velocity addition formula, the definition p=mu is not suitable to obtain conservation of momentum in special relativity!!
Need new definition for relativistic momentum!
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Conservation of Momentumy
x
u1
u2
m
m
If u1 = -u2 we find:ptot,before = 0ptot,after = 0
S
y'
x'
u'1
u'2
m
m
S'
System S' is moving to the right with the velocity v = u1x. We will use relativistic velocity transformations here.
u1x
u1y
Frame S’ moves along x with v = u1x
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Classical momentumy
u1=(ux,uy)
u2 = (-ux,-uy)
m
m
S
p1, before = m(ux , uy)p2, before = m(-ux , -uy)
p1, after = m(ux , -uy)p2, after = m(-ux , uy)
ptot , before = m(0 , 0)
ptot , after = m(0 , 0)
ptot , before = ptot, after
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Galileo (classical):
p1, before = m ( 0 , uy)p2, before = m (-2ux , -uy)
p1, after = m ( 0 , -uy)p2, after = m (-2ux , uy)
ptot , before = m (-2ux , 0)
ptot , after = m (-2ux , 0)
ptot , before = ptot, after
y'
x'
u'1
u'2
m
m
S'
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Velocity transformation (3D)
2/1'
cvuvuu
x
xx
2/1'
cvuu
ux
yy
2/1'
cvuuu
x
zz
Relativistic:Classical:
u'x = ux – v
u'y = uy
u'z = uz
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Lorentz transformation
ptot , before ≠ ptot, after
y'
x'
u'1
u'2
m
m
S'
2/1'
cvuvuu
x
xx
2/1'
cvuu
ux
yy
Use:
Algebra
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Conservation of momentum is extremely useful in classical physics. For the new definition of relativistic momentum we want:
1. At low velocities the new definition of p should match the classical definition of momentum.
2. We want that the total momentum (Σp) of an isolated system of bodies is conserved in all inertial frames.
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Relativistic momentum
Relativistic definition:
properdtdm rp
Classical definition:dtdm rp
Say we measure the mass 'm' in its rest-frame ('proper mass' or 'rest mass'). Since we measure 'm' it's rest-frame we agree on the same value for 'm' in all frames.
Assume we take the derivative with respect to the proper time tproper , which has the same meaning in all frames.
This definition fulfills the conservation of momentum in SR!
To prove it you can apply the relativistic velocity transformation.
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Relativistic momentum
The time dilation formula implies that dt = γdtproper We can therefore rewrite the definition of the relativistic momentum as follows:
urp mdtdm
An important consequence of the Lorentz-factor γ is, that no object can be accelerated past the speed of light.
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Example: Classical vs. Relativistic momentumAn electron has a mass m ≈ 9·10-31kg. The table below shows the classical and relativistic momentum of the electron at various speeds (units are 10-22kg·m/s):
u classical relativisticdifference
[%]0.1c 0.273 0.276 1.10.5c 1.36 1.57 15.40.9c 2.46 5.63 128.9
0.99c 2.7 19.2 611.1
p=m·u p=γm·u
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Relativistic momentum
p ⋅muA B
Particle A has half the mass but twice the speed of particle B. If the particles’ momenta are pA and pB, then
a) pA > pB
b) pA = pB
c) pA < pB
is bigger for the faster particle.