An empirical model for forecasting solar wind speed related geomagnetic events is presented here. The model is based on the estimated location and size of solar coronal holes. This method differs from models that are based on photospheric magnetograms (e.g., Wang-Sheeley model) to estimate the open field line configuration. Rather than requiring the use of a full magnetic synoptic map, the meth...

To forecast geomagnetic storms, we had examined initially observed parameters of coronal mass ejections (CMEs) and introduced an empirical storm forecast model in a previous study. Now we suggest a two-step forecast considering not only CME parameters observed in the solar vicinity but also solar wind conditions near Earth to improve the forecast capability. We consider the empirical solar wind...

Now a day‟s electricity is most needed facility for the human being. All the conventional energy resources are depleting day by day. So we have to shift from conventional to non-conventional energy resources. In this the combination of two energy resources is takes place i.e. wind and solar energy. This process reviles the sustainable energy resources without damaging the nature. Renewable ener...

[1] In this study, statistical evidence of a possible modulation of the equatorial stratospheric quasi‐biennial oscillation (QBO) by the solar wind dynamic pressure is provided. When solar wind dynamic pressure is high, the QBO at 30–70 hPa is found to be preferably more easterly during July–October. These lower stratospheric easterly anomalies are primarily linked to the high‐frequency compone...

The heliosphere is the bubble the Sun carves out of the interstellar medium. The solar wind moves outward at supersonic speeds and carries with it the Sun’s magnetic field. The interstellar medium is also moving at supersonic speeds and carries with it the interstellar magnetic field. The boundary between the solar wind and the interstellar medium is called the heliopause. Before these plasmas ...

In this paper we describe the development of two empirical models of Pc3 wave activity observed at a ground station. The models are tasked to predict pulsation intensity at Tihany, Hungary, from the OMNI solar wind data set at 5 min time resolution. One model is based on artificial neural networks and the other on multiple linear regression. Input parameters to the models are iteratively select...

The change in the magnetic energy stored in the Earth’s magnetotail as a function of the solar wind IMF conditions are investigated using an empirical magnetic field model. The results are used to calculate the two normal modes contained in the low-dimensional global model called WINDMI for the solar wind driven magnetosphere–ionosphere system. The coupling of the magnetosphere–ionosphere (MI) ...

Recent Ulysses observations from the Sun's equator to the poles reveal fundamental properties of the three-dimensional heliosphere at the maximum in solar activity. The heliospheric magnetic field originates from a magnetic dipole oriented nearly perpendicular to, instead of nearly parallel to, the Sun's rotation axis. Magnetic fields, solar wind, and energetic charged particles from low-latitu...

Analysis of previously reported observations of the solar wind-barium interaction associated with the AMPTE artificial comet release of December 27, 1984, is presented. On the basis of these results we argue that the solar wind couples momentum (and energy) to the barium ions through both laminar and turbulent processes. The laminar forces acting on the particles are the laminar electric and ma...

Physics of the Poynting-Robertson (P-R) effect is discussed and compared with the statements published in the past thirty years. Relativistically covariant formulation reveals the essence of the P-R effect and points out to nonphysical explanations in scientific papers and monographs. Although the final equation of motion m dv/dt = (SA ′ ¯ Q ′ pr / c) {(1 − v · e/c) e − v/c} has been usually co...