Sierpinski (<1K) Spacetime Kinematics and Mechanics

Energy and Momentum

    Just as a spacetime 1-vector "point" p decomposes into "time" p4 and "place" P =p1e1+p2e2+p3e3 when percieved by observer E, a timelike 1-vector four-momentum m=m1e1+m2e2+m3e3+m4e4 decomposes into "energy" m4 and "momentum" M=m1e1+m2e2+m3e3. We can measure energy and mass in m-1 and in the geometric algebra we can regard nonnull four-moentum 1-vectors as inverted nonnull spacetime displacements.
    With regard to a particular e4 it is natural to express timelike 1-vector m with m2=-m02 as
    m = m0(1-V2)(e4+V) = mE(e4 + V) where:

    Relative mass-energy mE is comprised of rest mass m0 plus an infinite series of positive kinetic energy terms in  m0V2k which for |V| << 1 are approximated by the first classical kinetic energy term ½m0V2 .

    A null 1-vector has zero proper mass but nonzero relative mass equal to the magnitude of its relative momentum. It is thus percieved as a relative mass m4 having unit relative velocity and consequent relative momentum m4V = ¯e4*(m) .  

    Let path P = { p(t) : t Î Â } be a proper worldline for a "particle" of constant proper mass m0 > 0 .
    Define xE : [t0,t1]   ® Â3,1 by xE(t) º ^(p(t),e4).
    Define tE : [t0,t1] ® Â by tE(t) º -e4¿p(t) so that ¯(p(t),e4) = tE(t)e4 .
    tE(t) is a monontonic increasing function of t so has an inverse function tE-1 : [tE(t0),tE(t1)] ® [t0,t1] such that tE-1(tE(t)) = t " t Î [t0,t1].
    The worldine of the particle can then be parameterised as P = { xE(tE-1(t)) + te4 : t Î [tE(t0),tE(t1)] } representing its perception by E.

    gE(t) º dtE(t) / dt   = (1 - vE(t)2) .
[ Proof :
(dp(t)/dt)2 = -1 Þ(dx(tE(t))/dt)2 - gE(t)2 = -1 Þ (dx(tE(t)/dt)2 = gE(t)2 - 1
Þ((dx(tE(t))/dtE(t) gE(t))2 = gE(t)2 - 1 ÞgE(t)2 = (1 - (dx(tE(t))/dtE(t))2)-1 .
ÞgE(t) = ± (1 - vE(t)2) where vE(t) = dxE(t)/dtE(t) is the relative velocity.
We take the + Ö  .]

    The e4-relative (forced Euclidean) modulus vv being the sum of "kinetic energy" (v1)2 +(v2)2 +(v3)2 and "mass energy" (v4)2 . is known as the Hamiltonian .
    v2   = (v1)2 + (v2)2 + (v3)2 - (v4)2   provides a measure refered to by physiscists as a Lagrangian .
    Some authors represent this split as e4m(t) = e4¿m(t) + e4Ùm(t) and consider the relative momentum to be a bivector but we do not take this approach here.
    EE(t) = -mEe42     (here = mE, elsewhere = mEc2).
    mE(t) = mEvE(t) .     [ Proof :  m0gE(t)vE(t) = m0 dtE(t)/dt dxE(t)/dtE(t) = m0 dxE(t)/dt  .]
    FE(t) º ^e4(p") is known as the relative force assumed acting on the particle.

    We can immediately derive two standard laws of Newtonian mechanics.

    Since gE(t) = (1 - vE(t)2) = 1 + ½vE2 + o(vE4) we have EE(t) » m0(1 + ½vE(t)2) for small |vE| , corresponding to   rest and kinetic energies.
    Note that though we use here the subscript E to denote relativity to an "observer" E, only e4 is actually relevant and coordinate independance within E's 3D spatial universe is retained.

Justifying E=mc2
    Einsteins most famous equation has emerged (as E=m) almost tautologically here from our identification of "rest mass-energy" with the magnitude of a four-momentum, so it is reassuring to follow Pearson and demonstrate it as independantly plausible other than implicitly from a Minkowski paradigm. In atomic decay we observe that on fragmenting into rapidly seperating elements, the total (inertial) mass of the assemblage is reduced while the total kinetic energy apparently increases. It is reasonable therefore to consider that some of the (inertial) mass of the particles has been transformed into kinetic energy. If we allow two seperate atoms to decay in a similar way the composite assemblage typically gains twice as much kinetic energy and looses twice as much mass as the single atom system so it is again plausable to assume a proportional relationship between matter and energy E = k m for some constant k.
    Consider accelerating a body of mass m from rest using a continuously applied 1-D "driver" force F we have
    F = (d/dt)(mv) = (d/dt)(kEv) = k(Edv/dt + vdE/dt)   =    k v dt/dx (Edv/dt + vdE/dt)   =    k v (Edv/dx + vdE/dx)
     Now, F dx is the ammount of work done and so should equal the gain in (kinetic) energy dE so we have
    dE   =   k v (Edv + vdE) Þ dE   =   k v E (1-kv2)-1 and so òE0EE-1 dE   =   ò0v dv(1-k2)-1 Þ ln(EE0-1) = -½ ln(1-kv2) Þ E = E0(1-kv2) and we see that energy E increases to infinity as v approaches upper limit k . Denoting this infinite energy requiring speed by c gives E = E0(1-(vc-1)2) and F = (d/dt)mv = c-2 Ev which integrates to mv = Evc-2 Þ E = mc2 .

    Alternatively we might follow Dmitriyev and consider a particle of mass M as a bubble of volume Vv of vapour in a turbulent fluid "either" of density rl and pressure Pl. The velocity of the particles in the volume Vl of fluid evapourating into the bubble has then form v= u0 + u where  u0 is the average drift over a short time interval and u is thermal jitter with <(u1)2> = <(u2)2> = <(u3)2> = c2 where <a> denotes averaging a over a small timeperiod and c2 is a measure of the thermal energy of the either. The net kinetic thermal energy inherited by the vapour is  
    ½rlVl( <(u1)2> + <(u2)2> + <(u3)2> ) = (3/2)rlVlc2 = (3/2)Mc2 where M=Mv=Ml is the mass of the vapourised fluid in the bubble.
    If the vapour is acting within the bubble as an ideal gas than the thermal energy of the vapour in the bubble is given by (3/2)PvVv so we have Mc2 = PvVv and since Pv=Pl for equilibrium we have E = PlVv = Mc2 as the work required to create the bubble against the fluid pressure Pl.

DeBroglie Waves

    Electrodynamic wave theory considers solutions of the Klein Gordan equation Ñp2yp = ± l2yp   , notably the normalised periodic solution  
    yp   =   y0eilp¿k º y0 (ilp¿k)     for p-independant null or unit timelike timelike 1-vector k and positive scalar l .
    Such waves are usually constucted over a Â1,3 timespace as complex-valued _cvpsi(X,t) e-i(wt - K.X)) so that (d/dt2 - ÑX2)_cvpsi = (w2 -K2)_cvpsi
    More generally,   yp   =   y0eilp¿k satisfies both yp»yp   =   y0»y0 and Ñp2yp = (-l2k2y0eilp¿k = l2yp for timelike unit k  or -l2yp for spacelike unit k. Because k2<0 the exponential power series for yp is "bounded trigonometric" rather than "divergent hyperbolic" .

    l is frequently expressed by physicists as 2pm0c/h with  m0= hl(2pc)-1 called the "mass" of y .
    In natural units c=1, h=(2p), h=1.
    Taking l = (2p)m0/h = ih-1m0 gives the traditional formulation (in our unorthodox notations) of the De Broglie Wave
    yp   =   y0(h-1m0(p¿k))   =   y0(h-1(p¿m))     for positive scalar m0 and unit timelike k with m = m0k .

    Relativisitically, an e4-observer percieves such a De Broglie wave vector h-1 m=m0k as splitting into positive scalar temporal wave frequency w=m0k4h-1 (and corresponding wave period 2p h (m0k4)-1 ) and spacial wave-vector h-1 ME = l-1¯e123(k)~ for wavelength l = h|ME|-1 .

    Energy E = m0k4 = hw   = m0(1+VE2)½ = m0(1 + ½VE2 - 1/8VE2 + ... + (-1)k4k(k-1)(2k(2k-1)(2k-2))-1 VE2k + ...

    Note the distinction between wave and particle energy "splits" here. Physicists traditionally "split" a particle four-momentum m=m0k as mEl(e4+V) but a wave four-momentum as hwe4 + hl-1 V~ for wave frequency w [  Often denoted v ] and wavelength l [  Often denoted l . ]
     The two V are distinct, one being spacial momentum divided by relative mass, the other the unscaled e123 projection. The kinetic energy series differ beyond the first, classical, term.  

    For a zero mass "electromagnetic" wave in a vacuum solving Ñp2yp = 0 ( ie. l=0) we have y0 (iap¿k)     for any nonzero a and nullvector k . The e4-relative frequency (energy) is then equal to the magnitude of the relative three-momentum hl-1 .

    Since h » 6.625×10-34 J s » 2-110 J s » 2-166 kg s , a visible wavelength photon of frequnecy 248 Hz has relative energy of order 2-62 J corresponding to relative mass 2-118 kg and we can multiply these values by factors ranging from 222 for gamma rays down to 2-17 for radio waves and remain within the recognised "electromagnetic spectrum".

    Since yp is is everywhere locally normalised,  we can interpret De Broglie wave y as a "particle" only if we regard it to be equiprobably distributed everywhere, ie. having a maximally ambiguous position which in a sense means not having a position at all. Wherever it "is", however, the "particle" has a predictable definite (wholly unambiguous) four-momentum m - at least until such time as we might attempt to observe the ambiguous position.

    Fixing t=e4¿p we note that yp is spacially periodic with directed wavelength h |¯e4*(m)|-1 ¯e4*(m)~ = h ME-2  ¯e4*(m)~ .

    Ðd yp = il(d¿k)yp   =   i2pmEh-1(d¿k)yp   =   -h-1mE(d¿k)yp
which is the Schrodinger wave equation with scalar multiplier Hamiltionian operator hp,d = -mE(d¿k) .

    With d=e4 we obtain Hamiltionian Hp = -e4¿m = mEk4 = mE(1 + vE2)½ [  k4 denotes coordinate e4¿k rather than |k|4 ] which for small vE2 we can approximate as mE(1 + ½ vE2 + O(vE4) + ...) corresponding to "rest" , "kinetic", and "higher order"  energies respectively.
    For "slow" De Brogle waves we thus have the non-relativistic approximation yp = y0(h-1mE(p¿vE - (1+½vE2 + O(vE4))t ) yp » (-h-1mE) y0(h-1mE(p¿vE - ½vE2t)
    We can incorporate the p-independant phase factor e-h-1mE into y0 to obtain yp » y0 (h-1mE(p¿vE - ½vE2t)) .

Relativistic Fluid Mechanics

Spacetime 1-flows
    Consider a nonunit timelike 1-vector valued field
    mp   =   mpup   =   Mp + mpe4   =   mp(1-Vp2)(Vp+e4)   =   mp(Vp+e4)   =   mpvp
at p as four-momentum due to matter of rest mass mp and unit 4D timelike "four-velocity" up.
    An e4-observer percieves mp as matter of relative mass mp º e4¿mp = mp(1-Vp2)     travelling at nonunit spacial velocity 1-vector Vp = ^e4(up) with relative momentum Mp = ^e4(mp) = mpVp . The matter conservation law becomes Ñp¿mp = 0 .
[ Proof :  Ñp¿mp = Ñ[e123]p¿mp + e4¿Ðe4mp = ÑP¿Mp + Ðe4(e4¿mp) = ÑP¿Mp + Ðe4mp = ÑP¿Mp + mp/t = 0  .]

    The e4-substantial derivative (vp¿Ñp)   =   Ðpvp   =   /x4 + (Vp¿Ñ[e123]) corresponds to that rate of change with respect to e4-time when following the e4-spacial flow Vp .
    For a static system (/x4 = 0) we have (vp¿Ñp)   =   (Vp¿ÑP)   =   ÐPVp .


    We likewise interpret a nonunit timelike 1-vector "current" field jp   =   jpup   =   rpup   =   Jp + j4pe4 as a 3D-current Jp and relative e4-charge j4  with charge conservation law
    Ñp¿jp   =   Ñ[e123]p¿Jp + j4p/ x4   =   0 . If jp falls away more slowly, eg. by a spacial r-1 factor then e4-charge may "radiate away". [ e4-dependant component j4p is often denoted r in the literature but we here retain r for the frame-independant magnitude rp = |jp| = jp. ]
    Ñp¿jp=0 ensures that j4 (sometimes refered to as the " probable charge" at p) is "globally conserved" over (e4-percieved) time in that its integration over a suitably large e4-cotemporal spacial volume remains constant over time, provided rp ® 0 faster than |p¿e123|-2 does as |p¿e123| ® ¥.
[ Proof : Fix e4¿p = t0 and consider a spacial 2-sphere St0 Ì  t0e4 + e4* of radius R . We postulate that rp ® 0 at any point on the surface of this sphere faster than R-2 as R becomes large (we assume the sphere still remains within Base) . This means that the Â3 boundary (spherical surface) integral òd St0 dp2 jp ® 0 as R ® ¥ and the geometric form of fundamental theorem of calculus (applied to Euclidean manifold St0) then provides that the scalar part of the volume integral ( òSt0 dp3 Ñp[St0] jp )<0> ® 0 as R ® ¥ . Other than at the boundary dSt0 , whose contribution to the volume integral we can neglect, Ñp[St0] = Ñp[e4*] and so the contribution to the volume integral of a small 3-simplex d3p at p is
(d3p Ñp[e4*]jp) = -(d3p Ñp[e4]jp) = -(e3e123  e4Ðe4 jp) = (e3e1234Ðe4 jp)
    Considering just the spacial (e123) component we obtain òSt0 dp3 Ðe4j4p » 0 Þ (d/dt) òSt dp3 j4p » 0 where the » indicates that we can get as close to zero as we wish by making R large enough. Hence the "total probable charge" within a large enough sphere is (effectively) constant   .  .]

    So if Ñp¿jp = 0 and |jp|® 0 sufficiently fast for large |d¿p| then - ò Wd,a d3p d¿jp is independant of a for any given unit timelike d and the percieved total relative charge is seen as constant by all inertial observers, though differing observers see differing constants.

    If Ñp¿jp =0 then we have the streamline identity
    (jp¿Ñp)jpÑ =  jp¿wp + Ñpjp2)     where wp = ÑpÙjp and jp=|jp| .
[ Proof :  ½Ñpjp2 = ½(ÑpjpÑjp + ÑpjpjpÑ)<1> = ½((Ñpjp)jp + Ñp(jpÑjp - 2jpÑÙjp))<1> = (Ñpjp).jp  - Ñp¿(jpÑÙjp) =   - Ñp¿(jpÑÙjp)
    = -jp¿wp + (Ñp¿jp)jpÑ - (Ñp¿jpÑ)jp) = -jp¿wp + (jp¿Ñp)jpÑ  .]

    For a static 3D flow with ÑP¿JP=0 we have classical Â3 form (JP¿ÑP)JP = (ÑP×JPJP + ÑPJP2) .

Probability Flows
    We sometimes interpret rx=|jx| as the probability of there being a particle of unit-charge or mass at x , the particle having, if present, four-velocity jx~  and e4-relative charge  j4|jx|-1 .

    For t=x4>R , the intersection of 3-tsphere O+-R,0 and the e4-cotemporal 2-plane We4,te4 = { p : e4¿p=x4=t} is a spacial 2-sphere of centre x4e4 and radius
    |X| = (t2-R2)½ = ((e4¿p)2 + p2)½ = |^e4(p)| , where p = Rp~ is any point in the intersection.
    rx is constant throughout We4,te4 Ç O+R,0 ,  since |x|=R=t cosh(c)-1 ; |X|=R sinh(c) = (t2-R2)½ ; x4=t ; x~4=tR-1 ; and ccosh-1(tR-1) all are.

    A more general approach is to define a 1-multiflow via a point-dependant directional 0-field Fp(a) such that scalar Fp(a) = Fp(a~) gives the ammount of matter at p flowing in direction a. For a timelike single flow mp we have Fp(a)=a-1¿mp = - a¿mp for timelike a and 0 for null or spacelike a.

    1-field flows are geometrically inadequate in that they encode only a four-direction and fail to embody the "internal freedoms" aka. the "spin" of constituent particles. We will require a multivector field yp to properly represent the "state of the matter" at a given p.
    An obvious generalisation of a 1-vector flow mp is a Â1,3 multivector-valued field mp defined over a 1-vector pointspace .   A "mass shell" normalisation condition mp2 = kp for some scalar field kp is satisfied by multivectors of the form mp = mp + mpe1234 provided mp2 = mp2 + kp.

    The Rigid body kinematics of UN carry readily into R3,1 as follows:   Let P = { p(t) : t Î [t0,t1] } be the proper time formulation of a worldline. Taking a4(t) = p'(t)~ = p'(t), we associate three (spacelike) orthonormal vectors a1(t),a2(t),a3(t) Î a4(t)* with each "particle event" p(t) corresponding to the spatial orientation of the particle.
    A = { A(t) = (a1(t),a2(t),a3(t),a4(t)) : t Î [t0,t1] } is thus an orthonormal 4D frame on a timelike curve and we call such a mobile.
    Because the mobile remains orthonormal, we can define a unique R3,1 unit rotor Rt satisfying Rt§(ai(t0)) = ai(t)     i=1,2,3,4 .
    Henceforth we will omitt writing (t) except occasionally for emphasis..
    We write A = R§(At0) º RAt0R§ .
    Given p(t0) and At0, these Rt completely specify the spacetime history of the orientated particle since p(t) = p(t0) + òt0ta4(s) ds .

    If A = R(At0) then A' = W.A where W º 2R'R§ is a pure bivector known as the proper angular velocity.
[ Proof : RR§=1 Þ R(R§)' = -R'R§ = -(R'R§)§ so R'R§ (and thus W) is a pure bivector.
    A' = (RAt0R§)' = R'At0R§ + RAt0(R§)' = R'R§A + AR(R§)' = R'R§A - A(R'R§) = (R'R§)×A = (2R'R§).A = W.A  .]

      In particular a4' = W.a4 Þ p" = W.p' . We also have p" = (p"Ùp').p' .
[ Proof : (p')2 = -1 Þ p"¿p' = 0 Þ p"p' = p"Ùp'. Hence p" = -(p'2)p" = -(p')(p'Ùp") = (p')(p"Ùp') = (p"Ùp').p'  .]

    So W = (p"Ùp') + b where b Î p'* is a pure bivector in a spacelike 3D subspace (and thus a 2-blade) rotationally accelerating the mobile around axis p'.

    It is natural to factor R as R=LRf4®a4 where Rf4®a4ºa4(f4+a4)~ and L is a "spatial" rotation satisfying L(a4) = a4.

Next : Spacetime Potential Theory

Glossary   Contents   Author
Copyright (c) Ian C G Bell 1999
Web Source: or
Latest Edit: 13 Jun 2014. Counter