The IMF is the magnetic field that originates from the Sun and is convected out into space by the solar wind. The solar wind is composed of ionized particles that move away from the Sun at supersonic speed (see

The Solar Wind Demonstration). As the magnetic field lines are entangled in the wind, they are convected outwards with it. We know from observations that, depending on the hemisphere and phase of the solar cycle, the magnetic field spirals inward or outward; the magnetic field follows the same shape of spiral in the northern and southern parts of the heliosphere, but with opposite field direction.

The form of this magnetic field is easy to derive if we make some preliminary assumptions. First of all, we assume steady-state (Parker 1958). Moreover, we assume that the solar gravitation and the acceleration of the solar wind flux can be neglected beyond some distance

, and so we can approximate the outward radial velocity as a constant

. The tangential component of the velocity,

, is given by the Sun's rotation. In ideal magneto-hydrodynamics, we assume that the plasma is a perfect conductor, that is, the interaction between the charged particles can be neglected relative to the much stronger interaction with the magnetic field. This implies that the magnetic field lines move with the plasma—in other words, they are "frozen" into the plasma, and thus the magnetic field streamlines are always parallel to the velocity streamlines.

For the 2D plot, we restrict the motion to the ecliptic plane and we obtain a differential equation for the radius

* *and the polar angle

. The integration of this differential equation gives the equation of the streamlines for the solar wind flow in polar coordinates. The dashed circles represent the orbits of several planets—the thickest one is the Earth orbit at (

a.u.). To get the 3D plot, we integrate the differential equation for

and

without imposing any restrictions on the angle

. We thus obtain the equation of the three-dimensional magnetic field streamlines (in spherical coordinates), for

km/s.

**Mathematical computations**The components of the velocity

are (in spherical coordinates):

where

is the angular velocity of the Sun. The field lines are assumed to corotate with the Sun's surface at

.

The differential equation for the velocity streamlines is obtained from

:

.

The equation is integrated from

to

and from

to

to get:

,

the equation of the 3D streamlines for the solar wind. The resulting 3D plot is shown for

km/s.

The dynamic 2D plot shows the two-dimensional spiral for

(ecliptic plane).

The gas that flows outwards from the Sun is threaded by the magnetic field lines that originate in the Sun. Because the gas (solar wind) is ionized, it will carry these embedded magnetic field lines with it. Therefore, these assumptions imply that the magnetic field streamlines correspond to the solar wind velocity streamlines.

The resulting plot shows that the IMF streamlines follow an Archimedean spiral, known as the Parker spiral. The Parker spiral is an ideal model—in reality, the radial velocity

is not a constant, but varies with the distance

from the Sun (see

The Solar Wind Demonstration). We can model the magnetic field of the Sun as a dipole field,

(Parker 1958). This is only an approximation and is valid only at a large distance from the Sun. However, the Parker model is a very good approximation of the magnetic field streamlines and it agrees with observations obtained from various satellites, such as Imp-1 (Wilcox and Ness 1965) or ISEE-1 and ISEE-3 (Russell et al. 1980). The Voyager 1 and 2 probes also confirmed the spiral-like structure of the IMF (e.g. Burlaga 1993).

C. T. Russell, G. L. Siscoe, and E. J. Smith, "Comparison of ISEE-1 and -3 Interplanetary Magnetic Field Observations,"

*Geophys. Res. Lett.*,

**7**(5), 1980 pp. 381–384.

J. M. Wilcox and N. F. Ness, "Quasi-Stationary Corotating Structure in the Interplanetary Medium,"

*J. Geophys. Res.*,

**70**(23), 1965 pp. 5793–5805.

L. F. Burlaga and N. F. Ness, "Radial and Latitudinal Variations of the Magnetic Field Strength in the Outer Heliosphere,"

*J. Geophys. Res.*,

**98**(A3), 1993 pp. 3539–3549.