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# New method to determine proton trajectories in the equatorial plane of a dipole magnetic field

*SpringerPlus***volume 4**, Article number: 130 (2015)

## Abstract

A parametric description of proton trajectories in the equatorial plane of Earth’s dipole magnetic field has been derived. The exact expression of the angular coordinate contains an integral to be performed numerically. The radial coordinate results from the initial conditions by basic mathematical operations and by using trigonometric functions. With the approximate angular coordinate formula, applicable for a wide variety of cases of protons trapped in Earth’s radiation belts, no numerical integration is needed. The results of exact and approximate expressions were compared for a specific case and small differences were found.

## Background

The differential equations of the motion of charged particles in a magnetic dipole field, as approximation of the Earth’s magnetic field, were derived already by Stőrmer (1907). Their solutions were obtained only numerically in an attempt to explain the behaviour of aurora borealis. The interest for charged particles trapped inside the dipole magnetic field increased by the discovery of Van Allen belts. A deep discussion of this topic can be found in Elliot (1963). Alfven (1950) developed an approximation splitting particle motion into guiding centre motion and gyration. The method has been enriched by Northrop (1961). Detailed studies of the motion of charged particles in the meridian plane of magnetic dipole fields are due to Markellos et al. (1978a) and (Markellos et al. 1978b).

The specific case of charged particle motion in the equatorial plane of the dipole magnet allowed De Vogelaere (1950) to obtain general periodic solutions of a Hill type differential equation from two numerically found particular solutions. Dragt (1964) in a comprehensive paper, describes a power series solution originating from a double power series solution of Stőrmer (1955). Graef and Kusaka (1938) obtained solutions for the motion in that plane in terms of elliptic integrals of first kind. These include a step of numerical calculation, no matter if the elliptic integral is obtained by a subroutine of the trajectory determining programme or if its value is picked up from tables.

Here parametric expressions of the proton coordinates in the equatorial plane were derived. Both exact radial and approximated angular coordinate expressions are strictly speaking, analytical formulas including only basic arithmetic operations and trigonometric functions. A prescribed accuracy for the angular coordinate is obtained from an exact formula by numerical integration, performed with the desired degree of precision.

## Results and discussion

### Radial coordinate-exact expression

We use a cylindrical coordinate system, Figure 1, with the polar coordinates r, θ in the equatorial plane of the dipole magnetic field (that of paper). Therefore, the z axis is directed along the dipole, the origin being located in its middle. A proton, moving with the velocity v_{0} in the equatorial plane will be pushed towards the origin if the magnetic field lines are directed to enter inside the paper, from outside the Earth’s body. In other words, we are looking at the figure from the Earth’s North magnetic pole. To determine the coordinate r we use two motion constants: the velocity v_{0} and the angular momentum, Eq. 3.35 from Miyamoto (2000), p.26.

“Point” means derivative with respect to the time.

c_{t} is a constant. q and m are the proton charge and mass respectively. A_{θ} is the only non vanishing vector potential component. For z = 0 this is:

with μ the Earth’s magnetic dipole moment.

Next we use Richardson’s (1947) parameter ψ, the angle between the velocity and the theta velocity component, by the substitution v_{θ} = v_{0}cosψ, earlier applied to describe ion paths in “wedge” magnetic fields and ion optical studies, see also Ioanoviciu (1989).

After substitution of A_{θ} and \( r\theta \) in (2) we have:

next we put:

and we obtain:

The constant c_{t} results from the initial conditions:

when the parameter takes the value ψ = ψ_{i}.

Eliminating c_{l}, between (6) and (8), next substituting r by ρ_{i} = r/ri we have:

where:

Two solutions for ρ_{i} result:

Only the solution with “plus” sign offers physically acceptable values.

From the above expressions we obtain the maxima and minima of the proton radial coordinate by derivation with respect to ψ. As ρ_{i} is a function ρ_{i}(cosψ) the derivative is

dρ_{i}/dψ = dρ_{i}/d(cosψ)(−sinψ) It vanishes for ψ = π and ψ = 2π values (if we limit to the first loop) that substituted in the solutions for ρ_{i} give the searched extreme values:

for cosψ = −1 ,

and

for cosψ = 1

Further radial coordinate expression simplification can be obtained if we select the observation starting point for ψ_{i} = π/2:

Here the index “i” has been removed.

Now ρ = r/r_{C}, η = μq/(p_{r}r_{C}
^{2}) with r_{C} the radial distance for ψ_{i} = π/2, p_{r} the relativistic particle momentum \( {p}_r={m}_0{v}_0/\sqrt{1-{\beta}^2}, \)

The extreme values of ρ are then:

We can use the simplified expressions by looking for an equivalent equation connecting r_{i} and η_{i} to r_{C} and η. By equating the maximum and the minimum of the equation (12), (13) to those of eq. (15), (16) we obtain the following equivalence:

The eq. (11) with “minus” sign, is identical with (14) if:.

and

The stability condition for the proton trajectories results from the equation of ρ. The condition to keep the charged particle trapped inside the dipole magnetic field: ρ must be real. This happens always if:

or by detailing η:

### Angular exact coordinate expression

The angular coordinate, θ is obtained by an integration to be performed numerically with the desired accuracy degree.

Finally we integrate over ψ from the beginning at ψ = π/2 to the current value of ψ:

### Approximating proton coordinates

Let’s estimate the η values for the Van Allen belts. For the Earth, dipole moment μ_{E} = 7.906×10^{15} T.m^{3}, equatorial radius R_{E} = 6.378×10^{6}m , the protons of 10÷100 MeV, moving inside the inner belt concentrated around 1.5R_{E,} have η = 188.536 to 58.247 (Hess 1962; Fiandrini et *al*. 2004).

For the protons of 1 MeV located between 2.5 and 8R_{E} (second belt) the values of η=215.147 and 21.01 while for those of 0.065 MeV η=844.087 and 82.43.

The enumerated η values suggest when the integral giving θ (as r values result straightforward) can be obtained with accuracy. We take the equation (9) and divide it by η. Accounting for 1/η as small quantity, we substitute 1/η = α and ρ = 1 + ε , both α and ε being assumed to be small quantities. Then we obtain:

That after the substitutions gives:

By successive approximation, we obtain the following expression for, ε after the third approximation step:

ρ obtained as 1 + ε has been substituted in the expression of dθ :

As dε has the form:

to obtain θ we have to integrate ψ from π/2 to the current ψ value.

After integration it results:

### Application to a specific case

The case of a trapped 60 MeV proton oscillating around the characteristic radial distance of 1.5 Earth radii was considered. The motion characterizing parameter results then to be η = 75.97. The exact coordinates ρ and θ, as well as the relative difference between the exact and the approximated angular coordinates (θ-θ_{app})/θ in percents were presented, for a complete loop, in Table 1. The error is of the order of 0.002% to 0.12%.

In Figure 2 the reduced radial distance r/r_{C} exact values were represented as function of θ_{app} in abscissa, for three consecutive complete loops, corresponding to the intervals, ψ = π/2 to 5π/2, ψ = 5π/2 to 9π/2 and ψ = 9π/2 to 13π/2 respectively.

## Conclusion

The coordinates of the protons moving in the Earth’s equatorial plane were derived as functions of a parameter. The use of the exact expressions assumes only basic operations and trigonometric functions to be involved for the radial coordinate calculation, while for the angular coordinate a numerical integration is necessary. Combining the exact radial formula with the approximated angular coordinate expression, an entirely analytic set of formulas has been obtained. The accuracy of this description has been shown on an illustrative example. The amazing simplicity of the coordinate expressions suggests possible developments by accounting for field perturbations.

## References

Alfven H (1950) Cosmical Electrodynamics. Oxford Clarendon Press, Oxford

De Vogelaere R (1950) Equation de Hill et problême de Stōrmer. Can J Math 2:440–456

Dragt AJ (1964) Trapped orbits in a magnetic dipole field. Rev Geophys 3:255–298

Elliot H (1963) The Van Allen particles. Rep Prog Phys 26:145–180

Fiandrini E, Esposito G, Bertucci B, Alpat B, Ambrosi G, Battista R, Burger WJ, Caraffini D, Di Masso L, Dinu N, Ionica M, Ionica R, Pauluzzi M, Menichelli M, Zuccon P (2004) Protons with kinetic energy E > 70 MeV trapped in the Earth’s radiation belts. J Geophys Res Space Physics 109:A10, DOI:10.1029/2004JA010394

Graef C, Kusaka S (1938) On periodic orbits in the equatorial plane of a magnetic dipole. J Math Phys 17:43–54

Hess WN (1962) Energetic particles in the inner Van Allen belt. Space Sci Rev 1:278–312

Ioanoviciu D (1989) Ion Optics. In: Hawkes PW (ed) Advances in Electronics and Electron Physics, vol 73. Academic, New York, pp 1–92

Markellos VV, Klimopoulos S, Halioulias AA (1978a) Periodic motion in the meridian plane of a magnetic dipole I. Celest Mech 17:215–232

Markellos VV, Klimopoulos S, Goudas C (1978b) Periodic motion in the meridian plane of a magnetic dipole II. Celest Mech 17:233–249

Miyamoto K (2000) Fundamentals of Plasma Physics and Controlled Fusion. NIFS-PROC-48. National Institute of Fusion Science, Tokyo

Northrop TG (1961) The guiding center approximation to charged particle motion. Ann Phys 15:79–101

Richardson HOW (1947) Magnetic focusing between inclined plane pole-faces. Proc Roy Soc 59:791–795

Stőrmer C (1907) Sur les trajectoires des corpuscules éléctrisés dans le champ d’un aimant élémentaire avec application aux auroras boréales. Arch Sci Phys Nat 24:175–186

Stőrmer C (1955) The Polar Aurora. Oxford at Clarendon Press, Oxford

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The author declares that he has no competing interests.

### Authors’ information

Damaschin Ioanoviciu retired.

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### Keywords

- Proton orbits
- Van Allen belts
- Trapped protons
- Dipole magnetic field
- Stability condition