On the low latitude ''negative bays'' in the afternoon sector

Polar electrojet and simultaneous geomagnetic disturbances on poleward side of auroral zone simultaneous with positive bay observations in auroral zon

The Development of the Forbush Decrease and the Geomagnetic Storm Fields

Relationships between Forbush decreases and associated geomagnetic storm characteristic

The auroral oval, the auroral substorm, and their relations with the internal structure of the magnetosphere

Interaction between ring current and neutral sheet causing magnetospheric instability and changes in polar auror

Auroral effects in the D region of the ionosphere

The possible effects are discussed of radiations and corpuscles on relatively short-term changes in the circulation of the atmosphere (the development of cellular patterns in the zonal westerly flow, leading to the formation of cyclones) and relatively long-term changes in climate

Solar wind disturbances in th outer heliosphere caused by successive solar flares from the same active region

Solar wind disturbances caused by successive flares from the same active region are traced to about 20 AU, using the modeling method developed by Hakamada and Akasofu (1982). It is shown that the flare-generated shock waves coalesce with the co-rotating interaction region of the interplanetary magnetic field, resulting in a large-scale magnetic field structure in the outer heliosphere. Such a structure may have considerable effects on the propagation of galactic cosmic rays

The structure of the solar plasma flow generated by solar flares

Geomagnetic storm characteristics for two-dimensional configuration of solar plasma flow generated by solar flare

Auroral kilometric radiation/aurora correlation

Auroral kilometric radiation (AKR) observations from the ISIS 1 topside sounder receiver were compared with visual auroral observations from the network of Alaskan all-sky camera stations. The goal was to relate AKR source region encounters to specific auroral forms on the same magnetic field line. Thirty-eight simultaneous data sets were identified and analyzed. In general, intense AKR was associated with bright auroral arcs and conditions of weak or no AKR corresponded to times when either no aurora or only a faint arc or weak diffuse aurora were observed. Five cases, when both intense AKR and bright visual aurora were present, were analyzed in detail. Complete electron density N sub e contours, from the satellite altitude down to the F region ionization peak, were obtained along N-S traversals of the AKR source region. In addition, the ISIS 1 orbital tracks were projected down the magnetic field lines to the auroral altitude and compared to auroral features on a map derived from the all sky camera images. Density cavities (regions where N sub e 100/cu cm) were encountered on each of these passes

The dynamics of the aurora. Part VII - Equatorward motions and the multiplicity of auroral arcs

Dynamic motions of Aurora 7 towards equato

Electrodynamics of the magnetosphere - Geomagnetic storms

Electrodynamics of interaction between solar plasma flow and magnetosphere producing geomagnetic storm

The Computation of the Magnetic Field of any Axisymmetric Current Distribution—with Magnetospheric Applications

It is shown that the vector potential A of the magnetic field of any axisymmetric electric current distribution can be expressed in the form ∑ A n (r) P 1 n (cos θ). This series is used to compute the field of two model magnetospheric ring currents; the field of one of these was previously determined by double integrations by Akasofu, Cain & Chapman. The calculation of the functions A n (r) does not require double integrations. The two sets of results are in good agreement. The first term in the series for A gives the external magnetic moment of the ring current. The magnetic field energy is calculated for the field as a whole and for each term in the series for A. The field isointensity lines are drawn, and also the field lines for the ring current and for its field combined with that of the geomagnetic dipole. They illustrate the considerable distortion of the field in the magnetosphere during magnetic storms. The series for A may also be helpful in calculating the paths of cosmic rays in the deformed magnetosphere. The numerical convergence of the results is improved by the use of CesÀro summation.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/72484/1/j.1365-246X.1966.tb03088.x.pd