Particle History and Proper Velocity

Previous section: Spacetime Maps.

Next sectionSpacetime Trigonometry.


The history of a material particle is a timelike curve  X = X(τ), as illustrated in the figure.

X(τ) ∆X ct ct+c∆t dX c dτ O


The path length
cτ of an interval X along the history is the proper time interval registered by a clock traveling with the particle. Hence,

          X̃  =  |X|2  ≈  (c τ)2 

          and, in the limit, |dX| = c dτ

The proper velocity V = V (τ) of a particle is defined by 

\[\Large{V\,\,\, = \,\,\,\frac{1}{c}\,\,\frac{{dX}}{{d\tau }}\,\,\, = \,\,\,\frac{{dt}}{{d\tau }}\,\, + \,\,\frac{1}{c}\,\,\frac{{d{\bf{x}}}}{{d\tau }}\,\,,}\]


which must be distinguished from the relative velocity  v = dx/dt in a given inertial system.


Exercise: Prove

\[\Large{V\,\,\, = \,\,\,\gamma \,\left( {1\,\, + \,\,\frac{{\bf{v}}}{c}} \right)\,\,,\,\,\,\,\,\,\,\,\,\,\,\,\gamma \,\,\, = \,\,\,\frac{{dt}}{{d\tau }}\,\,\, = \,\,\,\sqrt {1\,\, - \,\,\frac{{{{\bf{v}}^2}}}{{{c^2}}}} }\]


           
(Click here for a solution to this exercise.)


The proper velocity V of a free particle is constant, so its history is a straight line given by the equation

          X  =  X(τX(0)  =  Vcτ  =  Vcτ


0 free particle 2 history x cτ = c∆t/γ x₀ X₀ c∆t ∆t v X(τ) ⇔ X(t) ∆X free particle 1 history cτ = - ct₀ / γ cτ=0 ⇔ ct₀ (proper time = τ) (proper time = t) ct = 0 ⇔ ⇔ ct



The time axis of an inertial system is the history of a free particle at rest at the origin so that
proper time τ of another free particle can be associated with observer time t, and the position vector x for an event  X = ct + x  is the directed distance from the particle history to the event. From the discussion above and this last diagram, we can see the relationship between the proper time τ of particle 2 and the proper time t of particle 1. We just integrate γ dτ dt from 0 to τ. This is easy because for free particles γ is constant:

          γcτ  =  ct(τ) - ct(τ=0)  =  ct - ct0  (=  ct  in our diagram)



Similarly, 
the time axis of every inertial system can be identified with the history of a free particle.


For a given observer (free particle) the position x and time t of a given event X can (in principle) be determined by radar ranging with light signals, as illustrated in the figure below. Note that the event X is simultaneous with event X2 = ct. This geometric construction is Einstein’ s operational procedure for synchronizing clocks at distant events.


x X₃ = ct₃ x Observer's history X₁ = ct₁ X₂ = ct = ct + |x| = ct - |x| X = ct +


We (the observer) would send a light pulse at ct1 to be reflected at X and received at ct3. The intervals of the blue light paths are zero (lightlike), so we get

          ct  =  (ct3 + ct1) / 2               and               |x|  =  (ct3 - ct1) / 2 .


We can verify these formulas from the diagram or from the following expressions for the two light paths:

          (ct - ct1)2x2  =  0  =  (ct3 - ct)2x2                    |x|  =  ct - ct1  =  ct3 - ct .


Below is an interactive diagram showing our previous diagram in a different light. It takes a while to get used to the features of spacetime maps, to construct and read them properly, and to avoid jumping to incorrect conclusions. It is interesting how a simple minus sign in the definition of the spacetime interval can wreak such havoc on our intuitive expectations, because our reflex is naturally to see lengths in Euclidean fashion. For example, in the previous diagram, we see right angles and equal sides on triangles and may feel comfortable with that. However, even in that simple example, with its 3D feel, we may tend to forget that the observer is simply sitting at a lab table and reflecting a light flash from a mirror. 


The following diagram is a bit harder on the intuition and therefore worth the mental exercise. Now our lab table is sitting in a spaceship traveling in the positive x-direction with respect to an earth observer whose history is the numbered vertical time axis. The worldline of the lab table is the green line in the diagram. We send the flash of light towards the mirror in the nose of the ship. You can drag the event X3 (the end of the light pulse's round trip) with the mouse to see how the ship speed changes, as well as to check the γ factor (see the definition above) and the lab table's proper time τ, whose values are updated in the diagram's yellow boxes. Dragging X3 to the earth observer's history line takes the ship speed to zero and then this diagram corresponds to the previous diagram.




While using the interactive diagram, check out the following details:


          1. The only meaningful ship speeds are for v/< 1


          2.
Earth time of event X3 is always equal to the γ factor times the spaceship's proper time τ from the origin to X3
              This
time dilation will be discussed in the following pages.


          3. 
Move X3 to (ct,x) = (4,2), so the speed of the ship is c/2.

              It may not look like it, but
the red and green triangles are the same as in our previous diagram!
              The speed of light being the same to all observers means that
a lightlike line will make a 45° angle with the
              worldline of any observer
, even with the tilted green line of the lab table's history. The smallest appearing red
              triangle angle (near 
X1 where the light flash is emitted) and the largest appearing green triangle angle (near X3
              where
 the refelected flash returns to the ship's detector) are both 45° angles! In fact, the red and green
              triangles are
both right angled isosceles triangles sharing a common side from the spaceship's perspective,
              just as in the previous diagram, even though they look distorted in this diagram, because we are viewing things
              from the perspective of earth coordinates and clocks.

              Hence, the conclusions from our previous diagram still follow:

                        From the ship's perspective, the green triangle gives:

                                  cτ = cτ2 = (cτ3 + cτ1) / 2 = (3.46 + 0) / 2 = 1.73 = √3

                          |x|  =  (cτ3 - cτ1) / 2  =  cτ3 - cτ  =  cτ - cτ1  =  √3

                        From the earth observer's perspective:

                                  ct  =  (ct3 + ct1) / 2  =  (4 + 0) / 2  =  2

                          |x|  =  3 - 1  =  2  =  (ct3 - ct1) / 2  =  (4 - 0) / 2 


          4. Again, m
ove X3 to (ct,x) = (4,2), so the speed of the ship is c/2.


              From the earth observer's perspective, the light flash travels 3 space units of distance, then bounces back
              for one space unit of distance before getting detected at the emitter. Thus, the light flash travels a total of 
              4 units of space distance. Meanwhile, the spaceship has traveled only 2 units of space distance, which checks,
              since the ship is traveling half as fast as the light flash. 

          5. The spaceship's green history is a line of constant spacial coordinate (x = 0) in the ship's frame.
              We can lay out grid lines parallel to this line to show
the ship's spacial coordinate lines as seen on the 
              earth observer's spacetime map. From the diagram, it is easy to see if we call the angle on the map between 
              the ship's green history line and the earth's numbered vertical history line "
a", then tan a = v/c.


              The
X..X2 red line, from the way we constructed it (described under the previous diagram), is a line of
              constant time in the ship's coordinates, often called
a line of simultaneity for ship observers. By laying
              out lines parallel to it, we draw
lines of the ship's time coordinates as seen on the earth spacetime map.
              The symmetry of these
red and green ship's coordinate lines in the diagram tells us the red lines make
              the same angle "
a" with earth's x-axis as the green lines make with earth's ct-axis.


              To complete the grid construction,
we just need to know how far apart to draw the lines. We found a hint
              about that in detail 2 above. Because we can see the slope of the
ship's green history line on the earth's map
              is always
c/v, we can write the equation (in earth coordinates) of that green history line which passes through
              the origin as 
ct = (c/v)x. We'd like to find where to draw the red line corresponding to cτ = 1. If we correctly
              draw that one, all other lines will be easy to duplicate. We know (from the discussion in the previous 
              paragraph) that if
the slope of all the green ship coordinate lines is c/v, then the slope of all the red ship
              coordinate lines is
v/c on the earth map. To find the earth coordinates corresponding the ship coordinates 
              of (
cτ=1, x=0), calculate the spacetime interval between the origin and this point:

                        (cτ)2 - 02  =  1  =  (ct)2 - x2  =  (ct)2 - (vt)2  =  (ct)(1 - v2/c2)  =  (ct)2 / γ2  

                        ct  =  γ               and               x  =  vt  =  (v/cct  =  (v/cγ


             Notice we've verified the observation from detail 2 above. Now we have the slope and a point on 
the ship's
             green worldline
corresponding to (cτ=1, x=0), but in earth coordinates, so we can calculate the ct intercept of that
 
            line. Now plug the earth point (ct=γx=vγ/c) into the red line equation ct (v/cx + b to get its ct-axis intercept:

                        b  =  ct - (v/cx  =  γ - (v/c)vγ/c  =  γ (1 - v2/c2)  =  γ / γ2  =  1 / γ


             You might want to check out these numbers in the interactive diagram again. We follow
the ship's green
             worldline
 from the origin to a proper time of cτ=1. This corresponds to the earth coordinates of (ct=1.15, x=0.58)
             when the spaceship has a speed of
c/2. We verify again that the earth time ct is the γ factor times the spaceship's
             proper time
cτ. And the red line of simultaneity for cτ=1 hits the earth ct-axis at 1/γ. The interactive diagram
             draws the grid lines, based on these conclusions, using:

                       a  =  angle between green line and ct-axis  =  angle between red line and x-axis  =  Arctan(v/c).

                       i  =  integer ranging from - 25 to + 25 for 50 extra grid lines of each color.

                       Red lines connect earth map points from (0, i/γ)  to  (cos a, i/γ + sin a).

                       Green lines connect earth map points from (i/γ, 0)  to  (i/γ + sin a, cos a).


             The interactive diagram has buttons to turn ON & OFF the
red and/or green spaceship coordinate grid lines
             as seen on the earth observer's spacetime map. You could practice by reading off spaceship and earth
             coordinates for events
X1, X2, X3 and X. You could make a table of both sets of coordinates and compare
             various intervals to check that they are independent of which coordinates are used (invariant interval). 




Previous sectionSpacetime Maps.

Next section: Spacetime Trigonometry.


© David Hestenes 2005, 2014