Biquaternion formulation of relativistic tensor dynamics

Size: px
Start display at page:

Download "Biquaternion formulation of relativistic tensor dynamics"

Transcription

1 Juli, 8, 2008 To be submitted... 1 Biquaternion formulation of relativistic tensor dynamics E.P.J. de Haas High school teacher of physics Nijmegen, The Netherlands epjhaas@telfort.nl In this paper we show how relativistic tensor dynamics and relativistic electrodynamics can be formulated in a biquaternion tensor language. The treatment is restricted to mathematical physics, known facts as the Lorentz Force Law and the Lagrange Equation are presented in a relatively new formalism. The goal is to fuse anti-symmetric tensor dynamics, as used for example in relativistic electrodynamics, and symmetric tensor dynamics, as used for example in introductions to general relativity, into one single formalism: a specific kind of biquaternion tensor calculus. Keywords: biquaternion, relativistic dynamics, Lorentz Force Law, Lagrange Equation, Lagrangian Introduction We start with a quote. One can say that space-time model and kinematics of the Quaternionic Relativity are nowadays studc 2008 E.P.J. de Haas

2 Juli, 8, 2008 To be submitted... 2 ied in enough details and can be used as an effective mathematical tool for calculation of many relativistic effects. But respective relativistic dynamic has not been yet formulated, there are no quaternionic field theory; Q-gravitation, electromagnetism, weak and strong interactions are still remote projects. However, there is a hope that it is only beginning of a long way, and the theory will mature. (Yefremov 2005) We hope that the content of this paper will contribute to the project described by Yegremov. Quaternions can be represented by the basis (1, I, J, K). This basis has the properties II = JJ = KK = 1; 11 = 1; 1K = K1 = K for I, J, K; IJ = JI = K; JK = KJ = I; KI = IK = J. A quaternion number in its summation representation is given by A = a a 1 I + a 2 J + a 3 K, in which the a µ are real numbers. Biquaternions or complex quaternions in their summation representation are given by C = A + ib = (a 0 + ib 0 )1 + (a 1 + ib 1 )I + (a 2 + ib 2 )J + (a 3 + ib 3 )K = a a 1 I + a 2 J + a 3 K + ib ib 1 I + ib 2 J + ib 3 K, (1) in which the c µ = a µ + ib µ are complex numbers and the a µ and b µ are real numbers. The complex conjugate of a biquaternion C is given by C = A ib. The quaternion conjugate of a biquaternion is given by C = A + ib = (a 0 + ib 0 )1 (a 1 + ib 1 )I (a 2 + ib 2 )J (a 3 + ib 3 )K. (2) In this paper we only use the complex conjugate of biquaternions.

3 Juli, 8, 2008 To be submitted... 3 Biquaternions or complex quaternions in their vector representation are given by or by C µ = c 0 1 c 1 I c 2 J c 3 K, (3) C µ = [c 0 1, c 1 I, c 2 J, c 3 K] (4) We apply this to the space-time four vector of relativistic biquaternion 4-space R µ as R µ = ict1 r 1 I r 2 J r 3 K = ir 0 1 r 1 I r 2 J r 3 K. (5) The space-time distance s can be defined as R µ R µ, or giving R µ R µ = [ ict1, r 1 I, r 2 J, r 3 K] [ict1, r 1 I, r 2 J, r 3 K], (6) R µ R µ = c 2 t 2 1 r 2 11 r 2 21 r 2 31 = (c 2 t 2 r 2 1 r 2 2 r 2 3)1. (7) So we get R µ R µ = s1 with the usual s = c 2 t 2 r 2 1 r 2 2 r 2 3 = r 2 0 r 2 1 r 2 2 r 2 3 (8) providing us with a (+,,, ) signature.

4 Juli, 8, 2008 To be submitted... 4 Adding the dynamic vectors The basic definitions we use are quite common in the usual formulations of relativistic dynamics. We start with an observer who has a given three vector velocity as v, a rest mass as m 0 and an inertial mass m i = γm 0 with γ = ( 1 v 2 /c 2 ) 1. We use the Latin suffixes as abbreviations for words, not for numbers. So m i stands for inertial mass and U p for potential energy. The Greek suffixes are used as indicating a summation over the numbers 0, 1, 2 and 3. So P µ stands for a momentum four-vector with components p 0 = 1U c i, p 1, p 2 and p 3. The momentum three-vector is written as p and has components p 1, p 2 and p 3. We define the coordinate velocity four vector as V µ = d dt R µ = ic1 v 1 I v 2 J v 3 K = iv 0 1 v 1 I v 2 J v 3 K. (9) The proper velocity four vector on the other hand will be defined using the proper time t 0, with dt = γt 0, as iγc1 U µ = d R µ = d 1 dt 0 dtr µ = γv µ = γv 1 I γv γ 2 J. (10) γv 3 K The momentum four vector will be P µ = m i V µ = m 0 U µ. (11) We further define the rest mass density as ρ 0 = dm 0 dv 0, (12)

5 so with Juli, 8, 2008 To be submitted... 5 dv = 1 γ dv 0 (13) and the inertial mass density as we get ρ i = dm i dv ρ i = dm i dv = dγm 0 1 dv γ 0 (14) = γ 2 ρ 0. (15) The momentum density four vector will be defined as i 1 u c i1 ig 0 1 G µ = g 1 I g 2 J = g 1 I g 2 J, (16) g 3 K g 3 K in which we used the inertial energy density u i = ρ i c 2. For this momentum density four vector we have the variations G µ = d dv P µ = dm i dv V µ = ρ i V µ = γ 2 ρ 0 V µ = γρ 0 U µ = γg proper µ. (17) The four vector partial derivative µ will be defined as i 1 c t1 µ = 1 I 2 J. (18) R µ 3 K

6 Juli, 8, 2008 To be submitted... 6 The electrodynamic potential four vector will be defined as i 1 φ1 ia c 0 1 A µ = A 1 I A 2 J = A 1 I A 2 J. (19) A 3 K A 3 K The electric four current density will be given by icρ e 1 ij 0 1 J µ = J 1 I J 2 J = J 1 I J 2 J = ρ ev µ, (20) J 3 K J 3 K with ρ e as the electric charge density. Adding the dynamic vector products, scalars The dynamic Lagrangian density L can be defined as L = Ṽ ν G ν = (u i v g)1 = u 0 1 (21) and the accompanying Lagrangian L as L = Ṽ ν P ν = (U i v p)1 = 1 γ U 01, (22) with u 0 as the rest system inertial energy density and U 0 as the rest system inertial energy. The latter is the usual Lagrangian of a particle moving freely in empty space. The Lagrangian density of a massless electric charge density current in an electrodynamic potential field can be defined as L = J ν A ν = (ρ e φ J A)1. (23)

7 Juli, 8, 2008 To be submitted... 7 On the basis of the Lagrangian density we can define a four force density as f µ L R µ = µ L = µ u 0. (24) In the special case of a static electric force field, and without the densities, the field energy is U 0 = qφ 0 and the relativistic force reduces to the Coulomb Force F = U 0 = q φ 0. (25) Using L = Ṽ ν G ν this four force density can be written as f µ = µ Ṽ ν G ν. (26) We can define the absolute time derivative d dt perfect fluid like, space/field quantity through of a continuous, V µ µ = Ṽ µ µ = v + t 1 = d 1. (27) dt Thus we can define the mechanic four force density as f µ d dt G µ = (V ν ν )G µ = V ν ( ν G µ ), (28) using the fact that biquaternion multiplication is associative. Adding the dynamic vector products, tensors

8 Juli, 8, 2008 To be submitted... 8 The stress energy density tensor T ν µ can be given as T ν µ = Ṽ ν G µ and gives T ν µ = [ iv 0 1, v 1 I, v 2 J, v 3 K] ig 0 1 g 1 I g 2 J g 3 K = v 0 g 0 1 iv 1 g 0 I iv 2 g 0 J iv 3 g 0 K iv 0 g 1 I v 1 g 1 1 v 2 g 1 K v 3 g 1 J iv 0 g 2 J v 1 g 2 K v 2 g 2 1 v 3 g 2 I iv 0 g 3 K v 1 g 3 J v 2 g 3 I v 3 g 3 1 (29) Its trace is T νν = Ṽ ν G ν = L. In relativistic dynamics we have a usual force density definition through the four derivative of the stress energy density tensor ν T ν µ = f µ (30) or ν V ν G µ = f µ (31) We want to find out if these equations still hold in our biquaternion version of the four vectors, tensors and their products.

9 Juli, 8, 2008 To be submitted... 9 We calculate the left hand side and get for ν T ν µ = ν Ṽ ν G µ : [ i c t1, 1 I, 2 J, 3 K = ] v 0 g 0 1 iv 1 g 0 I iv 2 g 0 J iv 3 g 0 K iv 0 g 1 I v 1 g 1 1 v 2 g 1 K v 3 g 1 J iv 0 g 2 J v 1 g 2 K v 2 g 2 1 v 3 g 2 I iv 0 g 3 K v 1 g 3 J v 2 g 3 I v 3 g 3 1 i 1 c tv 0 g 0 1 i 1 v 1 g 0 1 i 2 v 2 g 0 1 i 3 v 3 g c tv 0 g 1 I 1 v 1 g 1 I 2 v 2 g 1 I 3 v 3 g 1 I 1 c tv 0 g 2 J 1 v 1 g 2 J 2 v 2 g 2 J 3 v 3 g 2 J 1 c tv 0 g 3 K 1 v 1 g 3 K 2 v 2 g 3 K 3 v 3 g 3 K = i( 1 c tv 0 g v 1 g v 2 g v 3 g 0 )1 ( 1 c tv 0 g v 1 g v 2 g v 3 g 1 )I ( 1 c tv 0 g v 1 g v 2 g v 3 g 2 )J ( 1 c tv 0 g v 1 g v 2 g v 3 g 3 )K (32)

10 Juli, 8, 2008 To be submitted Using the chain rule this leads to ν T ν µ = i( 1 c v 0 t g 0 + v 1 1 g 0 + v 2 2 g 0 + v 3 3 g 0 )1 ( 1 c v 0 t g 1 + v 1 1 g 1 + v 2 2 g 1 + v 3 3 g 1 )I ( 1 c v 0 t g 2 + v 1 1 g 2 + v 2 2 g 2 + v 3 3 g 2 )J ( 1 c v 0 t g 3 + v 1 1 g 3 + v 2 2 g 3 + v 3 3 g 3 )K i( 1( c tv 0 )g 0 + ( 1 v 1 )g 0 + ( 2 v 2 )g 0 + ( 3 v 3 )g 0 )1 ( 1( c tv 0 g 1 ) + ( 1 v 1 )g 1 + ( 2 v 2 )g 1 + ( 3 v 3 )g 1 )I ( 1( c tv 0 g 2 ) + ( 1 v 1 )g 2 + ( 2 v 2 )g 2 + ( 3 v 3 )g 2 )J ( 1( c tv 0 g 3 ) + ( 1 v 1 )g 3 + ( 2 v 2 )g 3 + ( 3 v 3 )g 3 )K This can be abbreviated to So = ( 1 c v 0 t + v v v 3 3 ) ( 1 c tv v v v 3 ) ig 0 1 g 1 I g 2 J g 3 K ig 0 1 g 1 I g 2 J g 3 K = (Ṽ ν ν )G µ + ( ν Ṽ ν )G µ (33) ν (Ṽ ν G µ ) = (Ṽ ν ν )G µ + ( ν Ṽ ν )G µ (34) ν T ν µ = (Ṽ ν ν )G µ + ( ν Ṽ ν )G µ. (35) We have Ṽ ν ν = d and if we assume the bare particle velocity dt continuity equation ν Ṽ ν = 0, then we get ν T ν µ = d dt G µ = f µ. (36)

11 Juli, 8, 2008 To be submitted Electrodynamic vector products If we apply this to the case in which we have a purely electromagnetic four momentum density G µ = ρ e A µ then we have and L = Ṽ ν G ν = Ṽ ν ρ e A ν = J ν A ν, (37) The relativistic force equation T ν µ = Ṽ ν G µ = J ν A µ. (38) ν T ν µ = (Ṽ ν ν )G µ + ( ν Ṽ ν )G µ. (39) can be given its electrodynamic expression as ν T ν µ = ( J ν ν )A µ + ( ν J ν )A µ. (40) If the charge density current continuity equation ν J ν = 0 can be applied, then this reduces to ν T ν µ = ( J ν ν )A µ = (J ν ν )A µ = J ν ( ν A µ ). (41) The electrodynamic force field tensor B ν ν is given by In detail this reads B ν µ = B ν µ = ν A µ. (42) [ i 1 c t1, 1 I, 2 J, 3 K ] i 1 c φ1 A 1 I A 2 J A 3 K = 1 c 2 t φ1 i 1 c 1φI i 1 c 2φJ i 1 c 3φK i 1 c ta 1 I 1 A A 1 K 3 A 1 J i 1 c ta 2 J 1 A 2 K 2 A A 2 I i 1 c ta 3 K 1 A 3 J 2 A 3 I 3 A 3 1 (43)

12 Juli, 8, 2008 To be submitted To see that this tensor leads to the usual EM force field biquaternion, we have to rearrange the tensor terms according to their biquaternionic affiliation, so arrange them according to the basis (1, I, J, K). This results in ( 1 c 2 t φ 1 A 1 2 A 2 3 A 3 )1 ( 2 A 3 3 A 2 + i 1 c 1φ + i 1 c ta 1 )I ( 3 A 1 1 A 3 + i 1 c 2φ + i 1 c ta 2 )J ( 1 A 2 2 A 1 + i 1 c 3φ + i 1 c ta 3 )K (44) This equals F µ = ν A ν 1 (B 1 i 1 c E 1)I (B 2 i 1 c E 1)J (B 3 i 1 c E 1)K = F 0 1 F 1 I F 2 J F 3 K. (45) For this biquaternion to be the exact match with the EM force field, one has to add the Lorenz gauge condition F 0 = ν A ν = 0. The operation of rearranging the tensor terms according to their biquaternion affiliation is external to the mathematical physics of this paper. We try to develop a biquaternion version of relativistic tensordynamics. The above operation destroys the tensor arrangement of the terms involved. It is alien to the system we try to develop in this context. It may be a useful operation in others areas though, for example in quantum physics. The electrodynamic force field tensor Bµ ν can also be given by B ν µ = µ A ν. (46) This leads to the same EM force field biquaternion.

13 Juli, 8, 2008 To be submitted The combination of Eq.(41) and Eq.(42) leads to ν T ν µ = J ν B ν µ, (47) which is valid if charge is conserved so if ν J ν = 0. We can write Eq.(41) also as ν T ν µ = ( J ν ν )A µ = ρ e (Ṽ ν ν )A µ = ρ d dt A µ. (48) The two EM force expression we gave in this and the previous sections based on f µ = ν T ν µ and f µ = µ L do not result in the well known Lorentz Force. But we can establish a relationship between these force expressions and the Lorentz Force. The Lorentz Force Law The Lorentz Force Law in its density form is given by the expression f µ = J ν ( ν A µ ) ( µ Ã ν )J ν, (49) or So if charge is conserved we also have f µ = J ν B ν µ ( µ Ã ν )J ν. (50) f µ = ν T ν µ ( µ Ã ν )J ν (51) as an equivalent. If we examen this last part ( µ Ã ν )J ν in more detail, an interesting relation arises. We begin with the equation µ L = µ J ν A ν. (52)

14 Juli, 8, 2008 To be submitted Now clearly we have J ν A ν = Ãν J ν = u 0 1 as a Lorentz invariant scalar. Together with the chain rule this leads to µ J ν A ν = ( µ J ν )A ν + ( µ Ã ν )J ν. (53) This equation is crucial for what is to come next, the connection of a Lagrange Equation to the Lorentz Force Law. So we have to prove it in detail, provide an exact proof, specially because biquaternion multiplication in general is non-commutative. We start the proof with µ Ã ν : µ Ã ν = i 1 c t1 1 I 2 J 3 K [ ia 01, A 1 I, A 2 J, A 3 K] = 1 c ta 0 1 i 1 c ta 1 I i 1 c ta 2 J i 1 c ta 3 K i 1 A 0 I 1 A A 2 K 1 A 3 J i 2 A 0 J 2 A 1 K 2 A A 3 I i 3 A 0 K 3 A 1 J 3 A 2 I 3 A 3 1 (54) In the next step we calculate ( µ Ã ν )J ν and use the fact that

15 Juli, 8, 2008 To be submitted ( 3 A 1 )J 2 = J 2 ( 3 A 1 ): ( µ Ã ν )J ν = 1 c ta 0 1 i 1 c ta 1 I i 1 c ta 2 J i 1 c ta 3 K i 1 A 0 I 1 A A 2 K 1 A 3 J i 2 A 0 J 2 A 1 K 2 A A 3 I i 3 A 0 K 3 A 1 J 3 A 2 I 3 A 3 1 [ij 0 1, J 1 I, J 2 J, J 3 K] = ( i 1J c 0 t A 0 + i 1J c 1 t A 1 + i 1J c 2 t A 2 + i 1J c 3 t A 3 )1 (J 0 1 A 0 J 1 1 A 1 J 2 1 A 2 J 3 1 A 3 )I (J 0 2 A 0 J 1 2 A 1 J 2 2 A 2 J 3 2 A 3 )J (55) (J 0 3 A 0 J 1 3 A 1 J 2 3 A 2 J 3 3 A 3 )K Now clearly ( µ Ã ν )J ν and ( µ J ν )A ν behave identical, only J and A have changed places, so ( µ J ν )A ν = ( i 1 c A 0 t J 0 + i 1 c A 1 t J 1 + i 1 c A 2 t J 2 + i 1 c A 3 t J 3 )1 (A 0 1 J 0 A 1 1 J 1 A 2 1 J 2 A 3 1 J 3 )I (A 0 2 J 0 A 1 2 J 1 A 2 2 J 2 A 3 2 J 3 )J (A 0 3 J 0 A 1 3 J 1 A 2 3 J 2 A 3 3 J 3 )K (56)

16 Juli, 8, 2008 To be submitted If we add them and use the inverse of the chain rule we get ( µ Ã ν )J ν + ( µ J ν )A ν = i 1( c tj 0 A 0 t J 1 A 1 t J 2 A 2 t J 3 A 3 )1 ( 1 J 0 A 0 1 J 1 A 1 1 J 2 A 2 1 J 3 A 3 )I ( 2 J 0 A 0 2 J 1 A 1 2 J 2 A 2 2 J 3 A 3 )J ( 3 J 0 A 0 3 J 1 A 1 3 J 2 A 2 3 J 3 A 3 )K i 1 c 1 1 I 2 J 3 K = (J 0A 0 J 1 A 1 J 2 A 2 J 3 A 3 ) = µ ( J ν A ν ) (57) Thus we have given the exact proof of the statement So we get µ J ν A ν = ( µ J ν )A ν + ( µ Ã ν )J ν. (58) µ L = µ J ν A ν = ( µ J ν )A ν + ( µ Ã ν )J ν. (59) We now have two force equations, fµ L = µ L = µ u 0 and fµ T = ν T ν µ = d G dt µ. We combine them into a force equation that representing the difference of these two forces: f µ = f T µ + f L µ = ν T ν µ + µ L. (60) For the purely electromagnetic case this can be written as and leads to f µ = ν J ν A µ µ J ν A ν (61) f µ = ( J ν ν )A µ + ( ν J ν )A µ ( µ J ν )A ν ( µ Ã ν )J ν. (62)

17 Juli, 8, 2008 To be submitted If we have ν J ν = 01 and µ J ν = 0 then this general force equation reduces to the Lorentz Force Law f µ = ( J ν ν )A µ ( µ Ã ν )J ν. (63) This of course also happens if ν J ν = µ J ν, so if the RHS of this equation has zero non-diagonal terms. The Lagrangian Equation If the difference between fµ T and fµ L is zero, we get the interesting equation ν T ν µ = µ L. (64) For the situation where µ Ṽ ν statement so we get which equals We will prove that = 0 we already proven the ν T ν µ = d dt G µ, (65) d dt G µ = µ L, (66) d dt G µ = L. (67) R µ G µ = Ṽ ν G ν = L, (68) see Appendix A for the proof and its limitations. Combined with the forgoing equation, this leads us to d dt ( L ) = L R µ (69)

18 as equivalent to Juli, 8, 2008 To be submitted ν T ν µ = µ L. (70) A canonical Lagrangian density If we choose a canonical Lagrangian density as L = Ṽ ν G ν + J ν A ν = v g J A u i + ρ e φ, (71) and an accompanying stress energy density tensor T ν µ = Ṽ ν G µ J ν A µ, (72) then our force equation f T µ = f L µ can be split in an inertial LHS and an EM RHS ( f T µ + f L µ ) inertial = ( f T µ + f L µ ) EM. (73) For situations were (f L µ ) inertial = µ u 0 = 0 this results in f inertial µ = f Lorentz µ. (74) as d dt G µ = J ν ( ν A µ ) ( µ Ã ν )J ν. (75) Maxwell s inhomogeneous equations We end with the formulation of the two inhomogeneous equations of the set of four Maxwell Equations, as they can be expressed in our terminology. They read ν ν A µ µ ν A ν = µ 0 J µ. (76)

19 Juli, 8, 2008 To be submitted It can be written as ( c 2 d 2 dt 2 )A µ µ ( t φ A) = µ 0 J µ, (77) so as the difference between a wave like part and the divergence of the Lorenz gauge part. Conclusions We have presented a specific kind of biquaternion relativistic tensor dynamics. We formulated the general equation ν T ν µ + µ L = 0. (78) The stress energy density tensor of a massive moving charged particle in a potential field was formulated as T ν µ = Ṽ ν G ν + J ν A ν with an accompanying Lagrangian density L as its trace L = T νν. Under curtain continuity conditions for the four current and the four velocity, this leads to the Lorentz Force Law and to the usual equations of relativistic tensor dynamics. One advantage of our specific kind of biquaternion formalism is that it is very akin to the usual relativistic space-time language. Acknowledgments I would like to thank xxx for valuable comments. Appendix A Proof We want to proof that, under curtain conditions, we have L = Ṽ ν G ν = G ν. (79)

20 Juli, 8, 2008 To be submitted The chain rule as we have used and shown before gives a first hunch. The chain rule leads us to Ṽ ν G ν = ( Ṽ ν )G ν + ( V Gν )V ν. (80) µ As before, we cannot assume this, because it uses commutativity, so we have to prove it. We start the proof with Ṽ ν : Ṽ ν = v 0 v 0 1 i v 1 v 0 I i v 2 v 0 J i v 3 v 0 K i v 0 1 v 1 I v 2 J v 3 K i v 0 v 1 I v 1 v 1 1 v 2 v 1 K v 3 v 1 J [ iv 01, v 1 I, v 2 J, v 3 K] = i v 0 v 2 J v 1 v 2 K v 2 v 2 1 v 3 v 2 I i v 0 v 3 K v 1 v 3 J v 2 v 3 I (81) v 3 v 3 1 Now we use the fact that we have an orthogonal basis, so v µ v ν = δ µν : Ṽ ν = 11 0I 0J 0K 0I 11 0K 0J 0J 0K 11 0I 0K 0J 0I 11 (82)

21 Juli, 8, 2008 To be submitted Then we multiply G ν with the result, giving 11 0I 0J 0K 0I 11 0K 0J 0J 0K 11 0I 0K 0J 0I 11 The result of this part is For the second part, ( Ṽ ν )G ν = [ig 01, g 1 I, g 2 J, g 3 K] = ig 0 1 g 1 I g 2 J g 3 K = G µ. (83) ( Ṽ ν )G ν = G µ. (84) ( Gν )V ν, (85) we have two options. The first is the easiest, assuming particle velocity and particle momentum to be independent properties, which makes this part zero and gives us the end result L = Ṽ ν G ν = ( Ṽ ν )G ν = G µ. (86) In the case that L = J ν A ν this assumption is allowed.

22 Juli, 8, 2008 To be submitted The second option is that particle velocity and particle momentum are mutually dependent through the relation G ν = ρ i V ν, with ρ i as the inertial mass density. In that case we have to go back to the original equation. If we assume a velocity independent mass density this gives L = Ṽ ν G ν = ρ (Ṽ ν V ν ) = ρ (v 2 0 v 2 1 v 2 2 v 2 3) = 2G µ. (87) The last situation is assumed in relativistic gravity, where the stress energy tensor is given by ρ i Ũ ν U ν. In that situation could be tempted to choose the Lagrangian as L = 1 2 ρ iũ ν U ν in order to preserve the outcome L = G ν. (88) This is done for example by Synge in his book on relativity (Synge, 1965, page 394). But that is outside our scope. So we have to restrict the use of L = Ṽ ν G ν = G ν (89) to the situations in which V µ and G µ are independent of each other. References [1] A.P. Yefremov, Quaternions and biquaternions: algebra, geometry, and physical theories. arxiv: mathph/ , 2005.

23 Juli, 8, 2008 To be submitted [2] J.L. Synge, Relativity: The Special Theory. North-Holland Pub. Co, Amsterdam, 2nd ed, 1965.

Biquaternion formulation of relativistic tensor dynamics

Biquaternion formulation of relativistic tensor dynamics Apeiron, Vol. 15, No. 4, October 2008 358 Biquaternion formulation of relativistic tensor dynamics E.P.J. de Haas High school teacher of physics Nijmegen, The Netherlands Email: epjhaas@telfort.nl In this

More information

Maxwell s equations. based on S-54. electric field charge density. current density

Maxwell s equations. based on S-54. electric field charge density. current density Maxwell s equations based on S-54 Our next task is to find a quantum field theory description of spin-1 particles, e.g. photons. Classical electrodynamics is governed by Maxwell s equations: electric field

More information

Classical Field Theory

Classical Field Theory April 13, 2010 Field Theory : Introduction A classical field theory is a physical theory that describes the study of how one or more physical fields interact with matter. The word classical is used in

More information

Special Relativity - QMII - Mechina

Special Relativity - QMII - Mechina Special Relativity - QMII - Mechina 2016-17 Daniel Aloni Disclaimer This notes should not replace a course in special relativity, but should serve as a reminder. I tried to cover as many important topics

More information

Lecture 13 Notes, Electromagnetic Theory II Dr. Christopher S. Baird, faculty.uml.edu/cbaird University of Massachusetts Lowell

Lecture 13 Notes, Electromagnetic Theory II Dr. Christopher S. Baird, faculty.uml.edu/cbaird University of Massachusetts Lowell Lecture 13 Notes, Electromagnetic Theory II Dr. Christopher S. Baird, faculty.uml.edu/cbaird University of Massachusetts Lowell 1. Covariant Geometry - We would like to develop a mathematical framework

More information

As usual, these notes are intended for use by class participants only, and are not for circulation. Week 7: Lectures 13, 14.

As usual, these notes are intended for use by class participants only, and are not for circulation. Week 7: Lectures 13, 14. As usual, these notes are intended for use by class participants only, and are not for circulation. Week 7: Lectures 13, 14 Majorana spinors March 15, 2012 So far, we have only considered massless, two-component

More information

Week 1. 1 The relativistic point particle. 1.1 Classical dynamics. Reading material from the books. Zwiebach, Chapter 5 and chapter 11

Week 1. 1 The relativistic point particle. 1.1 Classical dynamics. Reading material from the books. Zwiebach, Chapter 5 and chapter 11 Week 1 1 The relativistic point particle Reading material from the books Zwiebach, Chapter 5 and chapter 11 Polchinski, Chapter 1 Becker, Becker, Schwartz, Chapter 2 1.1 Classical dynamics The first thing

More information

FYS 3120: Classical Mechanics and Electrodynamics

FYS 3120: Classical Mechanics and Electrodynamics FYS 3120: Classical Mechanics and Electrodynamics Formula Collection Spring semester 2014 1 Analytical Mechanics The Lagrangian L = L(q, q, t), (1) is a function of the generalized coordinates q = {q i

More information

Week 1, solution to exercise 2

Week 1, solution to exercise 2 Week 1, solution to exercise 2 I. THE ACTION FOR CLASSICAL ELECTRODYNAMICS A. Maxwell s equations in relativistic form Maxwell s equations in vacuum and in natural units (c = 1) are, E=ρ, B t E=j (inhomogeneous),

More information

Gravitational radiation

Gravitational radiation Lecture 28: Gravitational radiation Gravitational radiation Reading: Ohanian and Ruffini, Gravitation and Spacetime, 2nd ed., Ch. 5. Gravitational equations in empty space The linearized field equations

More information

SPECIAL RELATIVITY AND ELECTROMAGNETISM

SPECIAL RELATIVITY AND ELECTROMAGNETISM SPECIAL RELATIVITY AND ELECTROMAGNETISM MATH 460, SECTION 500 The following problems (composed by Professor P.B. Yasskin) will lead you through the construction of the theory of electromagnetism in special

More information

Overthrows a basic assumption of classical physics - that lengths and time intervals are absolute quantities, i.e., the same for all observes.

Overthrows a basic assumption of classical physics - that lengths and time intervals are absolute quantities, i.e., the same for all observes. Relativistic Electrodynamics An inertial frame = coordinate system where Newton's 1st law of motion - the law of inertia - is true. An inertial frame moves with constant velocity with respect to any other

More information

A Method of Successive Approximations in the Framework of the Geometrized Lagrange Formalism

A Method of Successive Approximations in the Framework of the Geometrized Lagrange Formalism October, 008 PROGRESS IN PHYSICS Volume 4 A Method of Successive Approximations in the Framework of the Geometrized Lagrange Formalism Grigory I. Garas ko Department of Physics, Scientific Research Institute

More information

Microscopic electrodynamics. Trond Saue (LCPQ, Toulouse) Microscopic electrodynamics Virginia Tech / 46

Microscopic electrodynamics. Trond Saue (LCPQ, Toulouse) Microscopic electrodynamics Virginia Tech / 46 Microscopic electrodynamics Trond Saue (LCPQ, Toulouse) Microscopic electrodynamics Virginia Tech 2015 1 / 46 Maxwell s equations for electric field E and magnetic field B in terms of sources ρ and j The

More information

Stress-energy tensor is the most important object in a field theory and have been studied

Stress-energy tensor is the most important object in a field theory and have been studied Chapter 1 Introduction Stress-energy tensor is the most important object in a field theory and have been studied extensively [1-6]. In particular, the finiteness of stress-energy tensor has received great

More information

Maxwell s equations. Daniel Henry Gottlieb. August 1, Abstract

Maxwell s equations. Daniel Henry Gottlieb. August 1, Abstract Maxwell s equations Daniel Henry Gottlieb August 1, 2004 Abstract We express Maxwell s equations as a single equation, first using the divergence of a special type of matrix field to obtain the four current,

More information

Math. 460, Sec. 500 Fall, Special Relativity and Electromagnetism

Math. 460, Sec. 500 Fall, Special Relativity and Electromagnetism Math. 460, Sec. 500 Fall, 2011 Special Relativity and Electromagnetism The following problems (composed by Professor P. B. Yasskin) will lead you through the construction of the theory of electromagnetism

More information

Chapter 10 Operators of the scalar Klein Gordon field. from my book: Understanding Relativistic Quantum Field Theory.

Chapter 10 Operators of the scalar Klein Gordon field. from my book: Understanding Relativistic Quantum Field Theory. Chapter 10 Operators of the scalar Klein Gordon field from my book: Understanding Relativistic Quantum Field Theory Hans de Vries November 11, 2008 2 Chapter Contents 10 Operators of the scalar Klein Gordon

More information

Lecture 5: Sept. 19, 2013 First Applications of Noether s Theorem. 1 Translation Invariance. Last Latexed: September 18, 2013 at 14:24 1

Lecture 5: Sept. 19, 2013 First Applications of Noether s Theorem. 1 Translation Invariance. Last Latexed: September 18, 2013 at 14:24 1 Last Latexed: September 18, 2013 at 14:24 1 Lecture 5: Sept. 19, 2013 First Applications of Noether s Theorem Copyright c 2005 by Joel A. Shapiro Now it is time to use the very powerful though abstract

More information

Part I. Many-Body Systems and Classical Field Theory

Part I. Many-Body Systems and Classical Field Theory Part I. Many-Body Systems and Classical Field Theory 1. Classical and Quantum Mechanics of Particle Systems 3 1.1 Introduction. 3 1.2 Classical Mechanics of Mass Points 4 1.3 Quantum Mechanics: The Harmonic

More information

Linearized Gravity Return to Linearized Field Equations

Linearized Gravity Return to Linearized Field Equations Physics 411 Lecture 28 Linearized Gravity Lecture 28 Physics 411 Classical Mechanics II November 7th, 2007 We have seen, in disguised form, the equations of linearized gravity. Now we will pick a gauge

More information

2.4 Parity transformation

2.4 Parity transformation 2.4 Parity transformation An extremely simple group is one that has only two elements: {e, P }. Obviously, P 1 = P, so P 2 = e, with e represented by the unit n n matrix in an n- dimensional representation.

More information

A simple and compact approach to hydrodynamic using geometric algebra. Abstract

A simple and compact approach to hydrodynamic using geometric algebra. Abstract A simple and compact approach to hydrodynamic using geometric algebra Xiong Wang (a) Center for Chaos and Complex Networks (b) Department of Electronic Engineering, City University of Hong Kong, Hong Kong

More information

Dynamics of Relativistic Particles and EM Fields

Dynamics of Relativistic Particles and EM Fields October 7, 2008 1 1 J.D.Jackson, Classical Electrodynamics, 3rd Edition, Chapter 12 Lagrangian Hamiltonian for a Relativistic Charged Particle The equations of motion [ d p dt = e E + u ] c B de dt = e

More information

Lagrangian. µ = 0 0 E x E y E z 1 E x 0 B z B y 2 E y B z 0 B x 3 E z B y B x 0. field tensor. ν =

Lagrangian. µ = 0 0 E x E y E z 1 E x 0 B z B y 2 E y B z 0 B x 3 E z B y B x 0. field tensor. ν = Lagrangian L = 1 4 F µνf µν j µ A µ where F µν = µ A ν ν A µ = F νµ. F µν = ν = 0 1 2 3 µ = 0 0 E x E y E z 1 E x 0 B z B y 2 E y B z 0 B x 3 E z B y B x 0 field tensor. Note that F µν = g µρ F ρσ g σν

More information

etc., etc. Consequently, the Euler Lagrange equations for the Φ and Φ fields may be written in a manifestly covariant form as L Φ = m 2 Φ, (S.

etc., etc. Consequently, the Euler Lagrange equations for the Φ and Φ fields may be written in a manifestly covariant form as L Φ = m 2 Φ, (S. PHY 396 K. Solutions for problem set #3. Problem 1a: Let s start with the scalar fields Φx and Φ x. Similar to the EM covariant derivatives, the non-abelian covariant derivatives may be integrated by parts

More information

The Particle-Field Hamiltonian

The Particle-Field Hamiltonian The Particle-Field Hamiltonian For a fundamental understanding of the interaction of a particle with the electromagnetic field we need to know the total energy of the system consisting of particle and

More information

Electric and Magnetic Forces in Lagrangian and Hamiltonian Formalism

Electric and Magnetic Forces in Lagrangian and Hamiltonian Formalism Electric and Magnetic Forces in Lagrangian and Hamiltonian Formalism Benjamin Hornberger 1/26/1 Phy 55, Classical Electrodynamics, Prof. Goldhaber Lecture notes from Oct. 26, 21 Lecture held by Prof. Weisberger

More information

Maxwell s equations. electric field charge density. current density

Maxwell s equations. electric field charge density. current density Maxwell s equations based on S-54 Our next task is to find a quantum field theory description of spin-1 particles, e.g. photons. Classical electrodynamics is governed by Maxwell s equations: electric field

More information

Lorentz-covariant spectrum of single-particle states and their field theory Physics 230A, Spring 2007, Hitoshi Murayama

Lorentz-covariant spectrum of single-particle states and their field theory Physics 230A, Spring 2007, Hitoshi Murayama Lorentz-covariant spectrum of single-particle states and their field theory Physics 30A, Spring 007, Hitoshi Murayama 1 Poincaré Symmetry In order to understand the number of degrees of freedom we need

More information

Lecture notes for FYS610 Many particle Quantum Mechanics

Lecture notes for FYS610 Many particle Quantum Mechanics UNIVERSITETET I STAVANGER Institutt for matematikk og naturvitenskap Lecture notes for FYS610 Many particle Quantum Mechanics Note 20, 19.4 2017 Additions and comments to Quantum Field Theory and the Standard

More information

Covariant Electromagnetic Fields

Covariant Electromagnetic Fields Chapter 8 Covariant Electromagnetic Fields 8. Introduction The electromagnetic field was the original system that obeyed the principles of relativity. In fact, Einstein s original articulation of relativity

More information

Review and Notation (Special relativity)

Review and Notation (Special relativity) Review and Notation (Special relativity) December 30, 2016 7:35 PM Special Relativity: i) The principle of special relativity: The laws of physics must be the same in any inertial reference frame. In particular,

More information

Noether s Theorem. 4.1 Ignorable Coordinates

Noether s Theorem. 4.1 Ignorable Coordinates 4 Noether s Theorem 4.1 Ignorable Coordinates A central recurring theme in mathematical physics is the connection between symmetries and conservation laws, in particular the connection between the symmetries

More information

Quantum Field Theory Notes. Ryan D. Reece

Quantum Field Theory Notes. Ryan D. Reece Quantum Field Theory Notes Ryan D. Reece November 27, 2007 Chapter 1 Preliminaries 1.1 Overview of Special Relativity 1.1.1 Lorentz Boosts Searches in the later part 19th century for the coordinate transformation

More information

Number-Flux Vector and Stress-Energy Tensor

Number-Flux Vector and Stress-Energy Tensor Massachusetts Institute of Technology Department of Physics Physics 8.962 Spring 2002 Number-Flux Vector and Stress-Energy Tensor c 2000, 2002 Edmund Bertschinger. All rights reserved. 1 Introduction These

More information

Continuous symmetries and conserved currents

Continuous symmetries and conserved currents Continuous symmetries and conserved currents based on S-22 Consider a set of scalar fields, and a lagrangian density let s make an infinitesimal change: variation of the action: setting we would get equations

More information

Mechanics Physics 151

Mechanics Physics 151 Mechanics Physics 151 Lecture 4 Continuous Systems and Fields (Chapter 13) What We Did Last Time Built Lagrangian formalism for continuous system Lagrangian L Lagrange s equation = L dxdydz Derived simple

More information

Part III. Interacting Field Theory. Quantum Electrodynamics (QED)

Part III. Interacting Field Theory. Quantum Electrodynamics (QED) November-02-12 8:36 PM Part III Interacting Field Theory Quantum Electrodynamics (QED) M. Gericke Physics 7560, Relativistic QM 183 III.A Introduction December-08-12 9:10 PM At this point, we have the

More information

MULTIVECTOR DERIVATIVES WITH RESPECT TO FUNCTIONS

MULTIVECTOR DERIVATIVES WITH RESPECT TO FUNCTIONS MULTIVECTOR DERIVATIVES WITH RESPECT TO FUNCTIONS Note to avoid any confusion: The first paper dealing with multivector differentiation for physics, and in particular the concept of multivector derivatives

More information

Introduction to relativistic quantum mechanics

Introduction to relativistic quantum mechanics Introduction to relativistic quantum mechanics. Tensor notation In this book, we will most often use so-called natural units, which means that we have set c = and =. Furthermore, a general 4-vector will

More information

Mechanics Physics 151

Mechanics Physics 151 Mechanics Physics 151 Lecture 15 Special Relativity (Chapter 7) What We Did Last Time Defined Lorentz transformation Linear transformation of 4-vectors that conserve the length in Minkowski space Derived

More information

Symmetry and Duality FACETS Nemani Suryanarayana, IMSc

Symmetry and Duality FACETS Nemani Suryanarayana, IMSc Symmetry and Duality FACETS 2018 Nemani Suryanarayana, IMSc What are symmetries and why are they important? Most useful concept in Physics. Best theoretical models of natural Standard Model & GTR are based

More information

INTRODUCTION TO GENERAL RELATIVITY AND COSMOLOGY

INTRODUCTION TO GENERAL RELATIVITY AND COSMOLOGY INTRODUCTION TO GENERAL RELATIVITY AND COSMOLOGY Living script Astro 405/505 ISU Fall 2004 Dirk Pützfeld Iowa State University 2004 Last update: 9th December 2004 Foreword This material was prepared by

More information

CHAPTER 1. SPECIAL RELATIVITY AND QUANTUM MECHANICS

CHAPTER 1. SPECIAL RELATIVITY AND QUANTUM MECHANICS CHAPTER 1. SPECIAL RELATIVITY AND QUANTUM MECHANICS 1.1 PARTICLES AND FIELDS The two great structures of theoretical physics, the theory of special relativity and quantum mechanics, have been combined

More information

Explicit gauge covariant Euler Lagrange equation

Explicit gauge covariant Euler Lagrange equation Explicit gauge covariant Euler Lagrange equation Clinton L. Lewis a Division of Science and Mathematics, West Valley College, Saratoga, California 95070 Received 11 November 2008; accepted 22 May 2009

More information

Construction of Field Theories

Construction of Field Theories Physics 411 Lecture 24 Construction of Field Theories Lecture 24 Physics 411 Classical Mechanics II October 29th, 2007 We are beginning our final descent, and I ll take the opportunity to look at the freedom

More information

Relativistic Dynamics

Relativistic Dynamics Chapter 4 Relativistic Dynamics The most important example of a relativistic particle moving in a potential is a charged particle, say an electron, moving in an electromagnetic field, which might be that

More information

Lecture 8. September 21, General plan for construction of Standard Model theory. Choice of gauge symmetries for the Standard Model

Lecture 8. September 21, General plan for construction of Standard Model theory. Choice of gauge symmetries for the Standard Model Lecture 8 September 21, 2017 Today General plan for construction of Standard Model theory Properties of SU(n) transformations (review) Choice of gauge symmetries for the Standard Model Use of Lagrangian

More information

Exercises Symmetries in Particle Physics

Exercises Symmetries in Particle Physics Exercises Symmetries in Particle Physics 1. A particle is moving in an external field. Which components of the momentum p and the angular momentum L are conserved? a) Field of an infinite homogeneous plane.

More information

Classical Physics. SpaceTime Algebra

Classical Physics. SpaceTime Algebra Classical Physics with SpaceTime Algebra David Hestenes Arizona State University x x(τ ) x 0 Santalo 2016 Objectives of this talk To introduce SpaceTime Algebra (STA) as a unified, coordinate-free mathematical

More information

3 Quantization of the Dirac equation

3 Quantization of the Dirac equation 3 Quantization of the Dirac equation 3.1 Identical particles As is well known, quantum mechanics implies that no measurement can be performed to distinguish particles in the same quantum state. Elementary

More information

4/13/2015. Outlines CHAPTER 12 ELECTRODYNAMICS & RELATIVITY. 1. The special theory of relativity. 2. Relativistic Mechanics

4/13/2015. Outlines CHAPTER 12 ELECTRODYNAMICS & RELATIVITY. 1. The special theory of relativity. 2. Relativistic Mechanics CHAPTER 12 ELECTRODYNAMICS & RELATIVITY Lee Chow Department of Physics University of Central Florida Orlando, FL 32816 Outlines 1. The special theory of relativity 2. Relativistic Mechanics 3. Relativistic

More information

1 Lagrangian for a continuous system

1 Lagrangian for a continuous system Lagrangian for a continuous system Let s start with an example from mechanics to get the big idea. The physical system of interest is a string of length and mass per unit length fixed at both ends, and

More information

d 2 Area i K i0 ν 0 (S.2) when the integral is taken over the whole space, hence the second eq. (1.12).

d 2 Area i K i0 ν 0 (S.2) when the integral is taken over the whole space, hence the second eq. (1.12). PHY 396 K. Solutions for prolem set #. Prolem 1a: Let T µν = λ K λµ ν. Regardless of the specific form of the K λµ ν φ, φ tensor, its antisymmetry with respect to its first two indices K λµ ν K µλ ν implies

More information

NOETHER'S THEOREM AND GAUGE GROUPS

NOETHER'S THEOREM AND GAUGE GROUPS MAR 1965 % ncrc.nc.inuq IC/65/20 INTERNATIONAL ATOMIC ENERGY AGENCY INTERNATIONAL CENTRE FOR THEORETICAL PHYSICS NOETHER'S THEOREM AND GAUGE GROUPS C. A. LOPEZ 1965 PIAZZA OBERDAN TRIESTE IC/65/2O INTERNATIONAL

More information

Lorentz Transformations and Special Relativity

Lorentz Transformations and Special Relativity Lorentz Transformations and Special Relativity Required reading: Zwiebach 2.,2,6 Suggested reading: Units: French 3.7-0, 4.-5, 5. (a little less technical) Schwarz & Schwarz.2-6, 3.-4 (more mathematical)

More information

Tensors and Special Relativity

Tensors and Special Relativity Tensors and Special Relativity Lecture 6 1 Introduction and review of tensor algebra While you have probably used tensors of rank 1, i.e vectors, in special relativity, relativity is most efficiently expressed

More information

Relativistic Electrodynamics

Relativistic Electrodynamics Relativistic Electrodynamics Notes (I will try to update if typos are found) June 1, 2009 1 Dot products The Pythagorean theorem says that distances are given by With time as a fourth direction, we find

More information

Special Relativity. Chapter The geometry of space-time

Special Relativity. Chapter The geometry of space-time Chapter 1 Special Relativity In the far-reaching theory of Special Relativity of Einstein, the homogeneity and isotropy of the 3-dimensional space are generalized to include the time dimension as well.

More information

General Relativity (j µ and T µν for point particles) van Nieuwenhuizen, Spring 2018

General Relativity (j µ and T µν for point particles) van Nieuwenhuizen, Spring 2018 Consistency of conservation laws in SR and GR General Relativity j µ and for point particles van Nieuwenhuizen, Spring 2018 1 Introduction The Einstein equations for matter coupled to gravity read Einstein

More information

Particle Physics I Lecture Exam Question Sheet

Particle Physics I Lecture Exam Question Sheet Particle Physics I Lecture Exam Question Sheet Five out of these 16 questions will be given to you at the beginning of the exam. (1) (a) Which are the different fundamental interactions that exist in Nature?

More information

Problem 1(a): As discussed in class, Euler Lagrange equations for charged fields can be written in a manifestly covariant form as L (D µ φ) L

Problem 1(a): As discussed in class, Euler Lagrange equations for charged fields can be written in a manifestly covariant form as L (D µ φ) L PHY 396 K. Solutions for problem set #. Problem a: As discussed in class, Euler Lagrange equations for charged fields can be written in a manifestly covariant form as D µ D µ φ φ = 0. S. In particularly,

More information

Einstein Toolkit Workshop. Joshua Faber Apr

Einstein Toolkit Workshop. Joshua Faber Apr Einstein Toolkit Workshop Joshua Faber Apr 05 2012 Outline Space, time, and special relativity The metric tensor and geometry Curvature Geodesics Einstein s equations The Stress-energy tensor 3+1 formalisms

More information

Lectures April 29, May

Lectures April 29, May Lectures 25-26 April 29, May 4 2010 Electromagnetism controls most of physics from the atomic to the planetary scale, we have spent nearly a year exploring the concrete consequences of Maxwell s equations

More information

Tensor Calculus, Relativity, and Cosmology

Tensor Calculus, Relativity, and Cosmology Tensor Calculus, Relativity, and Cosmology A First Course by M. Dalarsson Ericsson Research and Development Stockholm, Sweden and N. Dalarsson Royal Institute of Technology Stockholm, Sweden ELSEVIER ACADEMIC

More information

Outline. Basic Principles. Extended Lagrange and Hamilton Formalism for Point Mechanics and Covariant Hamilton Field Theory

Outline. Basic Principles. Extended Lagrange and Hamilton Formalism for Point Mechanics and Covariant Hamilton Field Theory Outline Outline Covariant Hamiltonian Formulation of Gauge Theories J. 1 GSI Struckmeier1,, D. Vasak3, J. Kirsch3, H. 1 Basics:,, General Relativity 3 Global symmetry of a dynamical system Local symmetry

More information

Classical and Quantum Mechanics of a Charged Particle Moving in Electric and Magnetic Fields

Classical and Quantum Mechanics of a Charged Particle Moving in Electric and Magnetic Fields Classical Mechanics Classical and Quantum Mechanics of a Charged Particle Moving in Electric and Magnetic Fields In this section I describe the Lagrangian and the Hamiltonian formulations of classical

More information

NON-INERTIAL FRAMES IN SPECIAL RELATIVITY

NON-INERTIAL FRAMES IN SPECIAL RELATIVITY NON-INERTIAL FRAMES IN SPECIAL RELATIVITY A. Blato Creative Commons Attribution 3.0 License (208) Buenos Aires Argentina This article presents a new formulation of special relativity which is invariant

More information

Analytical Mechanics for Relativity and Quantum Mechanics

Analytical Mechanics for Relativity and Quantum Mechanics Analytical Mechanics for Relativity and Quantum Mechanics Oliver Davis Johns San Francisco State University OXPORD UNIVERSITY PRESS CONTENTS Dedication Preface Acknowledgments v vii ix PART I INTRODUCTION:

More information

Assignment 10. Arfken Show that Stirling s formula is an asymptotic expansion. The remainder term is. B 2n 2n(2n 1) x1 2n.

Assignment 10. Arfken Show that Stirling s formula is an asymptotic expansion. The remainder term is. B 2n 2n(2n 1) x1 2n. Assignment Arfken 5.. Show that Stirling s formula is an asymptotic expansion. The remainder term is R N (x nn+ for some N. The condition for an asymptotic series, lim x xn R N lim x nn+ B n n(n x n B

More information

Particle Physics. Michaelmas Term 2011 Prof. Mark Thomson. Handout 2 : The Dirac Equation. Non-Relativistic QM (Revision)

Particle Physics. Michaelmas Term 2011 Prof. Mark Thomson. Handout 2 : The Dirac Equation. Non-Relativistic QM (Revision) Particle Physics Michaelmas Term 2011 Prof. Mark Thomson + e - e + - + e - e + - + e - e + - + e - e + - Handout 2 : The Dirac Equation Prof. M.A. Thomson Michaelmas 2011 45 Non-Relativistic QM (Revision)

More information

What is spin? André Gsponer Independent Scientific Research Institute Box 30, CH-1211 Geneva-12, Switzerland

What is spin? André Gsponer Independent Scientific Research Institute Box 30, CH-1211 Geneva-12, Switzerland What is spin? arxiv:physics/030807v3 [physics.class-ph] 0 Sep 003 André Gsponer Independent Scientific Research Institute Box 30, CH- Geneva-, Switzerland e-mail: isri@vtx.ch ISRI-03-0.3 February, 008

More information

Getting started: CFD notation

Getting started: CFD notation PDE of p-th order Getting started: CFD notation f ( u,x, t, u x 1,..., u x n, u, 2 u x 1 x 2,..., p u p ) = 0 scalar unknowns u = u(x, t), x R n, t R, n = 1,2,3 vector unknowns v = v(x, t), v R m, m =

More information

B = 0. E = 1 c. E = 4πρ

B = 0. E = 1 c. E = 4πρ Photons In this section, we will treat the electromagnetic field quantum mechanically. We start by recording the Maxwell equations. As usual, we expect these equations to hold both classically and quantum

More information

Exercises in field theory

Exercises in field theory Exercises in field theory Wolfgang Kastaun April 30, 2008 Faraday s law for a moving circuit Faradays law: S E d l = k d B d a dt S If St) is moving with constant velocity v, it can be written as St) E

More information

RELATIVISTIC TRANSFORMATION OF MAGNETIC DIPOLE MOMENT

RELATIVISTIC TRANSFORMATION OF MAGNETIC DIPOLE MOMENT Progress In Electromagnetics Research B, Vol. 47, 63 78, 013 RELATIVISTIC TRANSFORMATION OF MAGNETIC DIPOLE MOMENT Alexander Kholmetskii 1, *, Oleg Missevitch, and Tolga Yarman 3, 4 1 Belarus State University,

More information

Tensors - Lecture 4. cos(β) sin(β) sin(β) cos(β) 0

Tensors - Lecture 4. cos(β) sin(β) sin(β) cos(β) 0 1 Introduction Tensors - Lecture 4 The concept of a tensor is derived from considering the properties of a function under a transformation of the corrdinate system. As previously discussed, such transformations

More information

Existence of Antiparticles as an Indication of Finiteness of Nature. Felix M. Lev

Existence of Antiparticles as an Indication of Finiteness of Nature. Felix M. Lev Existence of Antiparticles as an Indication of Finiteness of Nature Felix M. Lev Artwork Conversion Software Inc., 1201 Morningside Drive, Manhattan Beach, CA 90266, USA (Email: felixlev314@gmail.com)

More information

arxiv: v1 [math.ds] 18 Nov 2008

arxiv: v1 [math.ds] 18 Nov 2008 arxiv:0811.2889v1 [math.ds] 18 Nov 2008 Abstract Quaternions And Dynamics Basile Graf basile.graf@epfl.ch February, 2007 We give a simple and self contained introduction to quaternions and their practical

More information

Covariant electrodynamics

Covariant electrodynamics Lecture 9 Covariant electrodynamics WS2010/11: Introduction to Nuclear and Particle Physics 1 Consider Lorentz transformations pseudo-orthogonal transformations in 4-dimentional vector space (Minkowski

More information

Fundamental equations of relativistic fluid dynamics

Fundamental equations of relativistic fluid dynamics CHAPTER VI Fundamental equations of relativistic fluid dynamics When the energy density becomes large as may happen for instance in compact astrophysical objects, in the early Universe, or in high-energy

More information

From Gravitation Theories to a Theory of Gravitation

From Gravitation Theories to a Theory of Gravitation From Gravitation Theories to a Theory of Gravitation Thomas P. Sotiriou SISSA/ISAS, Trieste, Italy based on 0707.2748 [gr-qc] in collaboration with V. Faraoni and S. Liberati Sep 27th 2007 A theory of

More information

Curved spacetime and general covariance

Curved spacetime and general covariance Chapter 7 Curved spacetime and general covariance In this chapter we generalize the discussion of preceding chapters to extend covariance to more general curved spacetimes. 219 220 CHAPTER 7. CURVED SPACETIME

More information

Attempts at relativistic QM

Attempts at relativistic QM Attempts at relativistic QM based on S-1 A proper description of particle physics should incorporate both quantum mechanics and special relativity. However historically combining quantum mechanics and

More information

Vector and Tensor Calculus

Vector and Tensor Calculus Appendices 58 A Vector and Tensor Calculus In relativistic theory one often encounters vector and tensor expressions in both three- and four-dimensional form. The most important of these expressions are

More information

Properties of Traversable Wormholes in Spacetime

Properties of Traversable Wormholes in Spacetime Properties of Traversable Wormholes in Spacetime Vincent Hui Department of Physics, The College of Wooster, Wooster, Ohio 44691, USA. (Dated: May 16, 2018) In this project, the Morris-Thorne metric of

More information

Electromagnetic. G. A. Krafft Jefferson Lab Jefferson Lab Professor of Physics Old Dominion University TAADI Electromagnetic Theory

Electromagnetic. G. A. Krafft Jefferson Lab Jefferson Lab Professor of Physics Old Dominion University TAADI Electromagnetic Theory TAAD1 Electromagnetic Theory G. A. Krafft Jefferson Lab Jefferson Lab Professor of Physics Old Dominion University 8-31-12 Classical Electrodynamics A main physics discovery of the last half of the 2 th

More information

Particle Physics Lecture 1 : Introduction Fall 2015 Seon-Hee Seo

Particle Physics Lecture 1 : Introduction Fall 2015 Seon-Hee Seo Particle Physics Lecture 1 : Introduction Fall 2015 Seon-Hee Seo Particle Physics Fall 2015 1 Course Overview Lecture 1: Introduction, Decay Rates and Cross Sections Lecture 2: The Dirac Equation and Spin

More information

Physics 110. Electricity and Magnetism. Professor Dine. Spring, Handout: Vectors and Tensors: Everything You Need to Know

Physics 110. Electricity and Magnetism. Professor Dine. Spring, Handout: Vectors and Tensors: Everything You Need to Know Physics 110. Electricity and Magnetism. Professor Dine Spring, 2008. Handout: Vectors and Tensors: Everything You Need to Know What makes E&M hard, more than anything else, is the problem that the electric

More information

Particle Physics Dr. Alexander Mitov Handout 2 : The Dirac Equation

Particle Physics Dr. Alexander Mitov Handout 2 : The Dirac Equation Dr. A. Mitov Particle Physics 45 Particle Physics Dr. Alexander Mitov µ + e - e + µ - µ + e - e + µ - µ + e - e + µ - µ + e - e + µ - Handout 2 : The Dirac Equation Dr. A. Mitov Particle Physics 46 Non-Relativistic

More information

Quantum Field Theory Example Sheet 4 Michelmas Term 2011

Quantum Field Theory Example Sheet 4 Michelmas Term 2011 Quantum Field Theory Example Sheet 4 Michelmas Term 0 Solutions by: Johannes Hofmann Laurence Perreault Levasseur Dave M. Morris Marcel Schmittfull jbh38@cam.ac.uk L.Perreault-Levasseur@damtp.cam.ac.uk

More information

Introduction to Modern Quantum Field Theory

Introduction to Modern Quantum Field Theory Department of Mathematics University of Texas at Arlington Arlington, TX USA Febuary, 2016 Recall Einstein s famous equation, E 2 = (Mc 2 ) 2 + (c p) 2, where c is the speed of light, M is the classical

More information

Week 3: Renormalizable lagrangians and the Standard model lagrangian 1 Reading material from the books

Week 3: Renormalizable lagrangians and the Standard model lagrangian 1 Reading material from the books Week 3: Renormalizable lagrangians and the Standard model lagrangian 1 Reading material from the books Burgess-Moore, Chapter Weiberg, Chapter 5 Donoghue, Golowich, Holstein Chapter 1, 1 Free field Lagrangians

More information

Basic hydrodynamics. David Gurarie. 1 Newtonian fluids: Euler and Navier-Stokes equations

Basic hydrodynamics. David Gurarie. 1 Newtonian fluids: Euler and Navier-Stokes equations Basic hydrodynamics David Gurarie 1 Newtonian fluids: Euler and Navier-Stokes equations The basic hydrodynamic equations in the Eulerian form consist of conservation of mass, momentum and energy. We denote

More information

GRAVITATION F10. Lecture Maxwell s Equations in Curved Space-Time 1.1. Recall that Maxwell equations in Lorentz covariant form are.

GRAVITATION F10. Lecture Maxwell s Equations in Curved Space-Time 1.1. Recall that Maxwell equations in Lorentz covariant form are. GRAVITATION F0 S. G. RAJEEV Lecture. Maxwell s Equations in Curved Space-Time.. Recall that Maxwell equations in Lorentz covariant form are. µ F µν = j ν, F µν = µ A ν ν A µ... They follow from the variational

More information

Relativistic Kinematics

Relativistic Kinematics Chapter 3 Relativistic Kinematics Recall that we briefly discussed Galilean boosts, transformation going from one inertial frame to another one, the first moving with an infinitesimal velocity δv with

More information

Lorentzian elasticity arxiv:

Lorentzian elasticity arxiv: Lorentzian elasticity arxiv:1805.01303 Matteo Capoferri and Dmitri Vassiliev University College London 14 July 2018 Abstract formulation of elasticity theory Consider a manifold M equipped with non-degenerate

More information

A rotating charged black hole solution in f (R) gravity

A rotating charged black hole solution in f (R) gravity PRAMANA c Indian Academy of Sciences Vol. 78, No. 5 journal of May 01 physics pp. 697 703 A rotating charged black hole solution in f R) gravity ALEXIS LARRAÑAGA National Astronomical Observatory, National

More information

PRINCIPLES OF PHYSICS. \Hp. Ni Jun TSINGHUA. Physics. From Quantum Field Theory. to Classical Mechanics. World Scientific. Vol.2. Report and Review in

PRINCIPLES OF PHYSICS. \Hp. Ni Jun TSINGHUA. Physics. From Quantum Field Theory. to Classical Mechanics. World Scientific. Vol.2. Report and Review in LONDON BEIJING HONG TSINGHUA Report and Review in Physics Vol2 PRINCIPLES OF PHYSICS From Quantum Field Theory to Classical Mechanics Ni Jun Tsinghua University, China NEW JERSEY \Hp SINGAPORE World Scientific

More information