On the wave zone of synchrotron radiation

Bagrov, V.G.

doi:10.1107/S1600577518013644

research papers

JOURNAL OF
SYNCHROTRON
RADIATION

ISSN: 1600-5775

Volume 25| Part 6| November 2018| Pages 1619-1622

https://doi.org/10.1107/S1600577518013644

On the wave zone of synchrotron radiation

V. G. Bagrov ^a,^b ^*

^aTomsk State University, Lenin Avenue 36, 634050 Tomsk, Russia, and ^bInstitute of High Current Electronics, SB RAS, Akademichesky Avenue 4, 634055 Tomsk, Russia
^*Correspondence e-mail: bagrov@phys.tsu.ru

Edited by I. Lindau, SLAC/Stanford University, USA (Received 7 August 2018; accepted 25 September 2018; online 26 October 2018)

The extension of the wave zone of synchrotron radiation is studied.

Keywords: wave zone; synchrotron radiation.

1. Introduction

A theoretical study into the problem of the wave zone of synchrotron radiation was carried out by Sokolov et al. (1966 ; pp. 45–49). This research was published in English two years later (Sokolov & Ternov, 1968 ; pp. 34–37). Since then, for half a century, these results (concerning the issue of the wave radiation zone) have been considered as rigorously proven. Indeed, the proof given by Sokolov et al. (1966) and Sokolov & Ternov (1968) remains valid; however, the possibility of applying these reasonings to an estimation of the wave zone size has to be refined. This problem is the subject of the present work.

2. Theory and discussion

The radiation power W of a charged particle in classical electrodynamics is given by the expression

$[W = \oint_{{\bf s}}\,({\bf S}\,{\rm{d}}{\bf s}), \eqno(1)]$

where the surface $[{\bf s}]$ is a sphere with its center at the charge location, and the vector $[{\bf S}]$ is the Poynting vector,

$[{\bf S} = {{c} \over {4\pi}} \, \left[{\bf E}{\bf H}\right]. \eqno(2)]$

The electric $[{\bf E}]$ and magnetic $[{\bf H}]$ radiation fields of a point charge, determined with the help of Liénard–Wiechert potentials, can be written in the form

$[\eqalignno{ {\bf{E}}={{e}\over{R^{2}\left[ 1-({\bf{n}}\boldbeta)\right]^{3}} }&\left\{ (1-\beta^{\,2})({\bf{n}}-\boldbeta)+{{R}\over{c}} \left[ {\bf{n}} \big[ ({\bf{n}}-\boldbeta)\,{\dot{\boldbeta}}\big] \right] \right\}_{\vphantom{\Big|}} , \cr {\bf{H}} & = \left[{\bf{n}}{\bf{E}}\right], \qquad {\bf{n}} = {\bf{R}}/{R}. &(3)}]$

Here, $[{\bf v}]$ = $[c\boldbeta]$ , $[{\dot\boldbeta}]$ = $[{\rm{d}}\boldbeta/{\rm{d}}t]$ , is the charge velocity, $[{\bf R}]$ is the vector connecting the location point of the radiating charge to the observation point of radiation, e is the charge magnitude and c is the speed of light. In the right-hand sides of relations (3), all the quantities are regarded at the time instant τ determined by the condition

$[\tau+{{R(\tau)}\over{c}}=t. \eqno(4)]$

In particular, equation (4) implies

$[{{\partial{t}}\over{\partial\tau}} = 1-({\bf{n}}\boldbeta). \eqno(5)]$

When considering synchrotron radiation, the velocity and acceleration of a particle are mutually orthogonal, constant in absolute value, and belong to one and the same fixed plane. Let us select the following coordinate system (see Fig. 1). The origin of the coordinate system is chosen at the location point of the radiating charge. The x-axis is directed along the velocity of the electron, and the y-axis is directed toward the center of the circular trajectory. We choose the z-axis so that the coordinate system is right-handed (when the charge moves in a constant and uniform magnetic field, with the z-axis being parallel to the external magnetic field). The radius of a circular orbit of the radiating particle is denoted by ρ and is oriented along the y-axis of the given coordinate system. The angle formed by the x-axis and the vector $[{\bf R}]$ is denoted by α $[(0\,\leq\,\alpha\,\leq\,\pi)]$ , while the angle between the y-axis and the projection of the vector $[{\bf R}]$ onto the yz-plane is denoted by χ $[(0\,\leq\,\chi\,\lt\,2\pi)]$ . The surface element is given by $[{\rm{d}}{\bf s}]$ = $[{\bf R}R\,{\rm{d}}\Omega]$ , $[{\rm{d}}\Omega]$ = $[\sin\alpha\,{\rm{d}}\alpha\,{\rm{d}}\chi]$ .

Figure 1
Coordinate system.

Taking into account the above notation and equations (1) and (2), one easily obtains a well known expression (Sokolov et al., 1966; Sokolov & Ternov, 1968) for the instantaneous power of synchrotron radiation,

$[W = {{ce^{2}\beta^{\,4}}\over{4\pi\rho^{2}}} \int\limits_{0}^{\pi}\int\limits_{0}^{2\pi} \psi\sin\alpha\,{\rm{d}}\alpha\,{\rm{d}}\chi, \eqno(6)]$

where, in virtue of relations (4) and (5), the right- and left-hand sides of equation (6) are regarded at the radiation instant τ, with the following notation being used,

$[\eqalign{ \psi & = a_{0}(\beta\semi\alpha,\chi)+a_{1}(\beta\semi\alpha,\chi)\,k+a_{2}(\beta\semi\alpha,\chi)\,k^{\,2}_{\vphantom{\big|}}, \cr a_{0} & = {{ (\beta-\cos\alpha)^{2}+(1-\beta^{\,2})\sin^2\alpha\sin^2\chi }\over{ (1-\beta\cos\alpha)^{5}_{\vphantom{|}} }}, \cr a_{1} = & {{ 2\sin\alpha(\beta-\cos\alpha)\cos\chi }\over{ (1-\beta\cos\alpha)^{5} }}, \qquad a_{2} = {{\sin^{2}\alpha}\over{(1-\beta\cos\alpha)^{5}}}, } \eqno(7)]$

$[k = {{1-\beta^{\,2}} \over {\beta}} \, {{\rho} \over {R}}. \eqno(8)]$

The expression in equation (7) is a second-order polynomial in the parameter k with three coefficients, $[a_{s}(\beta\semi\alpha,\chi)]$ (s = 0, 1, 2), depending on the value of β and on the integration angles $[\alpha,\chi]$ . For $[R\rightarrow\infty]$ [according to equation (8), this corresponds to the limit $[k\rightarrow0]$ ], the given expression results in the instantaneous angular distribution $[a_{0}(\beta\semi\alpha,\chi)]$ of synchrotron radiation power.

Formally, the value of k in equation (7) is an expansion parameter, and therefore by Sokolov et al. (1966) and Sokolov & Ternov (1968) we investigated the region $[k\,\lt\,1]$ , with the tacit assumption that this is the radiation wave zone. However, the smallness of the parameter k and the definition of the wave zone are related only indirectly: the parameter k may be small, but the wave zone has not yet been formed.

Let us point out two obvious facts: (a) the specific structure of the coefficients $[a_{s}(\beta\semi\alpha,\chi)]$ may alter the conclusion about the boundaries of the wave radiation zone; however, this structure was not investigated by Sokolov et al. (1966) and Sokolov & Ternov (1968); (b) if we consider radiation in a certain cone (the cone is given by the region of integration with respect to $[\alpha,\chi]$ ), then the wave zone is determined not only by the radiation properties but also by the choice of the cone in question. This fact was not considered by Sokolov et al. (1966) and Sokolov & Ternov (1968) either.

Let us examine the total power of synchrotron radiation. Substituting the expressions (7) and (8) into equation (6), we carry out integration over $[\alpha,\chi]$ in the entire space. As a result of simple calculations, we find

$[\eqalign{ W & = W_{0}\Phi_{0}, \qquad W_{0}={{2ce^{2}\beta^{\,4}}\over{3\rho^{2}\left(1-\beta^{\,2}\right)^{2}_{\vphantom{\big|}}}}, \cr \Phi_{0} & = 1+{\overline{k}}^{\,2}, \qquad \overline{k}=\left({{1-\beta^{\,2}}\over{\beta^{\,2}}}\right)^{\!1/2} {{\rho}\over{R}}. } \eqno(9)]$

Here, W₀ is the total emitted power in the limit $[R\rightarrow\infty]$ (Sokolov et al., 1966; Sokolov & Ternov, 1968), and the coefficient $[\overline{k}]$ characterizes the size of the near-field zone.

We assume the space region $[\overline{k}\,\lt\,1]$ to be the radiation wave zone. From equations (8) and (9) it then follows that k and $[\overline{k}]$ are related by

$[\gamma k = \overline{k}, \qquad \gamma = {{1}\over{\left(1-\beta^{\,2}\right)^{1/2}}}, \eqno(10)]$

where γ is the relativistic factor (assuming, for instance, the electron energy to be ∼1 GeV, we obtain for the relativistic factor the approximation $[\gamma\simeq2000]$ ). Equation (10) implies that $[k\,\lt\,\,\overline{k}]$ , and also the fact that $[\overline{k}\,\lt\,1]$ is not necessarily the case at $[k\,\lt\,1]$ . Consequently, the condition $[k\,\lt\,1]$ , discussed by Sokolov et al. (1966) and Sokolov & Ternov (1968), is a necessary one, but is not sufficient to determine the synchrotron radiation wave zone ( $[k\,\lt\,\,\overline{k}\,\lt\,1]$ ).

From equation (9), it follows that

$[\overline{k}\,=\,{{R_{v}}\over{R}}, \qquad R_{v}\,=\,\left({{1-\beta^{\,2}}\over{\beta^{\,2}}}\right)^{\!1/2}\!\!\rho \,=\, {{\rho}\over{\left(\gamma^{2}-1\right)^{1/2}}}, \eqno(11)]$

where R_v is the distance separating the radiation space into the wave zone ( $[R_{v}\,\lt\,\,R]$ ) and the near-field zone ( $[R_{v}\,\gt\,R]$ ). The classical theory (Sokolov et al., 1966; Sokolov & Ternov, 1968) predicts a relation between the orbit radius ρ, the velocity of the radiating particle and the strength H of the controlling external magnetic field,

$[\rho\,=\,\left({{\beta^{\,2}}\over{1-\beta^{2}}}\right)^{\!1/2} \, \, {{m_{0}c^{2}}\over{|eH|}}\,=\,\left(\gamma^{2}-1\right)^{1/2} \,\,\, {{m_{0}c^{2}}\over{|eH|}}, \eqno(12)]$

where m₀ is the rest mass of the radiating particle. Substituting the expression (12) into equation (11), we obtain R_v in the form

$[R_{v} = {{m_{0}c^{2}}\over{|eH|}} = {{c}\over{\omega_{\rm{c}}}}, \qquad \omega_{\rm{c}} = {{|eH|}\over{m_{0}c}}, \eqno(13)]$

where $[\omega_{\rm{c}}]$ is the cyclotron frequency. For instance, the field H = 1 T = 10⁴ electromagnetic CGS units results in R_v = 0.1704 cm. The expression (13) shows that the parameter R_v is determined only by the rest energy of the radiating particle and by the magnitude of the external magnetic field. The other characteristics (for example, speed) of the radiating particle do not influence the quantity R_v.

Let us consider two examples when the radiation cone does not cover the entire space.

As a first example, we represent the whole space as the sum of two $[(\pm)]$ subspaces: the subspace (-) is given by the region $[y\,\geq\,0]$ (which corresponds to $[\cos\chi\,\geq\,0]$ , and the center of the orbit lies in this subspace); the subspace (+) is given by the region $[y\,\lt\,0]$ (which corresponds to $[\cos\chi\,\lt\,0]$ , and the center of the orbit does not lie in this subspace). It is easy to obtain the expressions

$[\eqalign{ W_{(\pm)} & = W_{0}\Phi_{(\pm)}, \cr \Phi_{(\pm)} & = {{1}\over{2}}\left(1+{\overline{k}}^{2}\mp{{3\beta}\over{8}}\,\overline{k}\right), \cr \Phi_{0} & = \Phi_{(+)}+\Phi_{(-)}. } \eqno(14)]$

As expected, the particle characteristics (being its speed β) now also enter the expressions (14) for $[\Phi_{(\pm)}]$ ; however, the condition $[\overline{k}\,\lt\,1]$ determines the wave radiation zone in this case as well.

As a second example, we represent the entire space as the sum of two, (in) and (out), subspaces: the (in)-subspace corresponds to the radiation value $[(\boldbeta{\bf S})\,\gt\,0]$ (which determines the range of variation $[0\,\lt\,\,\alpha\,\lt\,\pi/2]$ ); the (out)-subspace corresponds to the radiation value $[(\boldbeta{\bf S})\,\lt\,\,0]$ (which determines the range of variation $[\pi/2\,\lt\,\,\alpha\,\lt\,\,\pi]$ ). Thus, the space is divided into the (in)-part, in which the projection of the radiation pulse on the particle velocity is positive, and the (out)-part, in which the projection of the radiation pulse on the particle velocity is negative.

For the (in)-subspace, it is easy to obtain expression

$[\eqalign{ & W_{(\rm{in})}=W_{0}\Phi_{(\rm{in})}, \qquad \Phi_{(\rm{in})}=\Phi_{(\rm{in})}^{0}(\beta)\left[1+A_{(\rm{in})}(\beta)\,{\overline{k}}^{2}\right]_{\vphantom{\big|}}, \cr& \Phi_{(\rm{in})}^{0}(\beta)= {{16+\beta(3+\beta^{\,2})(7-3\beta^{\,2})}\over{32_{\vphantom{|}}}}, \cr& A_{(\rm{in})}(\beta)= {{2(8-9\beta+3\beta^{\,2})(1+\beta)}\over{16-11\beta+6\beta^{\,2}-3\beta^{\,3}}}. } \eqno(15)]$

We note the simplest properties of the functions $[\Phi_{(\rm{in})}^{0}(\beta)]$ and $[A_{(\rm{in})}(\beta)]$ in the segment $[0\,\leq\,\beta\,\leq\,1]$ . The function $[\Phi_{(\rm{in})}^{0}(\beta)]$ increases monotonously,

$[\Phi_{(\rm{in})}^{0}(0) = {{1}\over{2}}\,\leq\,\Phi_{(\rm{in})}^{0}(\beta)\,\leq\,1 = \Phi_{(\rm{in})}^{0}(1), \eqno(16)]$

and the function $[A_{(\rm{in})}(\beta)]$ at the ends of the segment A_(in)(0) = A_(in)(1) = 1 has a unique maximum at the point

$[\eqalign{ \beta_{\rm{\max}} & = {{3-\sqrt{5}}\over{2_{\vphantom{\big|}}}} \simeq 0.38197, \cr A_{(\rm{in})}(\beta_{\rm{\max}}) & = {{10(18\sqrt{5}-5)}\over{319}}\simeq1.2617. } \eqno(17)]$

Thus, the variation domain of the function $[A_{(\rm{in})}(\beta)]$ is bounded,

$[1\,\leq\, A_{(\rm{in})}(\beta)\,\leq\,{{10(18\sqrt{5}-5)}\over{319}}\simeq1.2617. \eqno(18)]$

Returning to the expressions (15) and taking into account equations (16)–(18), we obtain

$[W_{(\rm{in})} = \left\{ \matrix{ {\textstyle{{1}\over{2}}}\,W_{0}\Phi_{0}\hfill & {\rm{non\hbox{-}relativistic\,\,limit}}\,\,(\beta \ll 1), \hfill \cr & \cr W_{0}\Phi_{0}\hfill & {\rm{ultra\hbox{-}relativistic\,\,limit}}\,\,(1\ll\gamma). \hfill } \right. \eqno(19)]$

From equation (19) we find that in the non-relativistic case half of the emtted energy falls on the (in)-subspace, whereas in the ultra-relativistic case this subspace accumulates all the emitted energy. The emergence condition for the wave zone still has the form $[\overline{k}\,\lt\,1]$ .

For the (out)-subspace, we obtain the expression

$[\eqalignno{ & W_{(\rm{out})}=W_{0}\Phi_{(\rm{out})}, \qquad \Phi_{(\rm{out})}=\Phi_{(\rm{out})}^{0}(\beta)\left[1+A_{(\rm{out})}(\beta)k^{\,2}\right]_{\vphantom{\big|}}, \cr & \Phi_{(\rm{out})}^{0}(\beta)={{16-\beta(3+\beta^{2})(7-3\beta^{2})}\over{32_{\vphantom{|}}}}, &(20)\cr& A_{(\rm{out})}(\beta) = {{2(8+9\beta+3\beta^{2})}\over{(1+\beta)(16+11\beta+6\beta^{2}+3\beta^{3})}}. }]$

From equations (15) and (20), it follows that $[\Phi_{0}]$ = $[\Phi_{(\rm{in})}+\Phi_{(\rm{out})}]$ , which corresponds to the equality of the total radiation energy to the sum of the two energies in the subspaces. This also means 1 = $[\Phi_{(\rm{in})}^{0}(\beta)+\Phi_{(\rm{out})}^{0}(\beta)]$ , which indicates that the radiation energy in the wave zone is equal to the sum of the two energies in the wave zone of the subspaces. The functions $[\Phi_{(\rm{out})}^{0}(\beta)]$ and $[A_{(\rm{out})}(\beta)]$ in the segment $[0\,\leq\,\beta\,\leq\,1]$ are bounded and monotonously decreasing functions of β,

$[{{1}\over{2}}\,\geq\,\Phi_{(\rm{out})}^{0}(\beta)\,\geq\, 0, \qquad 1\,\geq\,A_{(\rm{out})}(\beta)\,\geq\,{{5}\over{9}}\,. \eqno(21)]$

In the non-relativistic limit $[(\beta\ll1)]$ , as implied by equations (21) and (19), we find W_(out) = W_(in) = $[({1}/{2})W_{0}\Phi_{0}]$ [in this case, with allowance made for equation (10), it has been taken into account that k = $[\overline{k}]$ ].

In the ultra-relativistic limit $[(1\ll\gamma)]$ for $[A_{(\rm{out})}(\beta\sim1)]$ ≃ 5/9, with account taken of equation (20), we find

$[\Phi_{(\rm{out})} = \Phi_{(\rm{out})}^{0}(\beta\simeq1)\left(1+{{5}\over{9}}\,k^{2}\right), \eqno(22)]$

which differs significantly from the expression (9) involving k. Equation (22) involves k, and in this case the wave zone emerges earlier than in equation (9). However, as noted above, the limit $[\Phi_{(\rm{out})}^{0}(\beta\simeq1)\rightarrow0]$ holds true, and, according to equation (20), this results in $[\Phi_{(\rm{out})}(\beta\simeq1)\rightarrow0]$ . Consequently, the radiation value W_(out) in the ultra-relativistic limit is extremely small in relation to W_(in) and does not offer any tangible contribution to the total radiation.

For a given external magnetic field H in the ultra-relativistic limit, the radiation value W_(out) is not only small in relation to W_(in) but also tends to zero as the energy of the radiating charge increases. Indeed, taking into account equation (9) for the quantity W₀ and using equation (12), we find the expression

$[W_{0} = {{2e^{2}\beta^{\,2}\omega_{\rm c}^{2}} \over {3c(1-\beta^{\,2})}} = {{2e^{2} \omega_{\rm c}^{2}} \over {3c}}(\gamma^{2}-1), \eqno(23)]$

which implies that the radiation value W₀ [and thereby also the value of W_(in)] for some fixed H (with a fixed $[\omega_{\rm{c}}]$ ) increases infinitely with an increasing charge energy ( $[\sim\!\gamma^{2}]$ ). For W_(out) in equation (20), we obtain

$[\eqalign{ W_{(\rm{out})} & = {{e^{2}\omega_{\rm{c}}^{2}} \over {c}}\beta^{\,2}(1-\beta ^{\,2}) \, B_{(\rm{out})}(\beta) \, \left [1+A_{(\rm{out})}(\beta)k^{\,2}\right]_{\vphantom{\big|}}, \cr B_{(\rm{out})}(\beta) & = {{16+11\beta+6\beta^{2}+3\beta^{3}}\over{48(1+\beta)^{2}}}.} \eqno(24)]$

The value of $[B_{(\rm{out})}(\beta)]$ , decreasing monotonously in the segment $[0\,\leq\,\beta\,\leq\,1]$ , is bounded: $[{{1}/{3}}\,\geq\, B_{(\rm{out})}(\beta)\,\geq\,{{3}/{16}}]$ . From equation (24), it follows that a fixed H results in a radiation value W_(out) decreasing to zero as the energy $[(\sim\!\gamma^{-2})]$ increases.

3. Conclusions

It has been shown that the wave zone of synchrotron radiation is determined by the condition $[\overline{k}\,\lt\,1]$ [expressions (9) or (11)], which differs from the condition of Sokolov et al. (1966) and Sokolov & Ternov (1968).

Funding information

This work was supported in part by RFBR grant No. 18-02-00149 and by the Program for Improving TSU's Competitiveness among World Leading Scientific and Educational Centers.

References

Sokolov, A. A. & Ternov, I. M. (1968). Synchrotron Radiation, p. 202. Berlin: Academie-Verlag. Google Scholar
Sokolov, A. A., Ternov, I. M. & Bagrov, V. G. (1966). The Synchrotron Radiation, edited by A. A. Sokolov and I. M. Ternov, pp. 18–71. Moscow: Nauka. (In Russian.) Google Scholar

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JOURNAL OF
SYNCHROTRON
RADIATION

ISSN: 1600-5775

Volume 25| Part 6| November 2018| Pages 1619-1622

https://doi.org/10.1107/S1600577518013644

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research papers\(\def\hfill{\hskip 5em}\def\hfil{\hskip 3em}\def\eqno#1{\hfil {#1}}\)

On the wave zone of synchrotron radiation

1. Introduction

2. Theory and discussion

3. Conclusions

Funding information

References

research papers