Kinematic models of the interplanetary magnetic field

Abstract

Abstract. Current knowledge on the description of the interplanetary magnetic field is reviewed with an emphasis on the kinematic approach as well as the analytic expression. Starting with the Parker spiral field approach, further effects are incorporated into this fundamental magnetic field model, including the latitudinal dependence, the poleward component, the solar cycle dependence, and the polarity and tilt angle of the solar magnetic axis. Further extensions are discussed in view of the magnetohydrodynamic treatment, the turbulence effect, the pickup ions, and the stellar wind models. The models of the interplanetary magnetic field serve as a useful tool for theoretical studies, in particular on the problems of plasma turbulence evolution, charged dust motions, and cosmic ray modulation in the heliosphere.

The Structure of the Large-Scale Heliosphere as Seen by Current Models

“…It should be noted that many authors (e.g. Owens and Forsyth 2013 ; Lhotka and Narita 2019 ) do not refer to the general form of Equation ( 5 ), but rather its frequently used special case of constant in the limit , to wit as the ‘Parker spiral field’, with the latter authors even (wrongly) criticizing Parker’s model for not recognizing the sign reversal of the dipolar magnetic field across the two hemispheres. This sign reversal, however, is easily included by prescribing, say, , and Parker ( 1958 ) actually does mention as a possible choice to represent the solar dipole.…”

Dynamics of charged dust in the orbit of Venus

“…( 3) does not include time-dependent effects, such as variations in the axial tilt or the solar cycle. However, it is based on the classical Parker spiral including the axial tilt of the solar dipole with respect to the ecliptic (Lhotka & Narita 2019). The approach is therefore only valid on secular timescales, that is, where time-dependent effects due to solar activity are canceled because of averaging.…”

“…The approach is therefore only valid on secular timescales, that is, where time-dependent effects due to solar activity are canceled because of averaging. For additional information, see Lhotka & Narita (2019).…”

Radio Astronomical Tools for the Study of Solar Energetic Particles I. Correlations and Diagnostics of Impulsive Acceleration and Particle Propagation

“…The authors concluded that field lines rooted in active regions often have constant latitude out to about 0.3 AU, as predicted by the Parker model, but bend at larger distance and become approximately parallel to the ecliptic plane. No detailed comparison seems to have been undertaken so far with models including a latitudinal component of the heliospheric magnetic field, which have been developed to account for unusual magnetic connections traced by energetic particles (see the reviews by Smith, 2008;Owens and Forsyth, 2013;Lhotka and Narita, 2019).…”