Effect of solar wind plasma parameters on space weather

Abstract

Today's challenge for space weather research is to quantitatively predict the dynamics of the magnetosphere from measured solar wind and interplanetary magnetic field (IMF) conditions. ::: Do ::: you ::::: mean : A cCorrelative studies between the Ggeomagnetic Sstorms (GMSs) and the various interplanetary (IP) field/plasma parameters have been performed to search for the causes of geomagnetic activity and developing models for predictioning of the occurrence of GMSs, which are important for space weather predictions. In the present paper weWe foundfind a possible co-relation ofbetween geomagnetic stormGMSs withand solar wind and IMF parameters in three different situations and also derived the linear relation equation for all parameters in three situations. : ? On the basis of the present statistical study, we developed an empirical model. With the help of this model, we can predict all categories of geomagnetic stormGMSs. ::: Do ::: you ::::: mean This model is based on the following fact. T: the total interplanetary magnetic fieldIMF B total can be used asto trigger an alarm offor geomagnetic stormGMSs, when sudden changes in total magnetic field B total occur., itThis is athe first alarm on condition for a storm's arrival. It is observed in the present study that the southward B z-component of the IMF is an important factor for describing geomagnetic stormGMSs. And it is theA result of the paper is that the magnitude of B z is maximum neither during the initial phase (at the instant of the IP shock) nor during the main phase (at the instant of Disturbance storm time (Dst) minimum). : ? So iIt is seen in this study that there is a time delay between the maximum value of southward B z and the Dst minimum, and this time delay can be used in the prediction of the intensity of a magnetic storm two-three hours before ofthe main phase of a geomagnetic stormGMS. :: Do :::: you ::::: mean : A linear relation havehas been derived between the maximum value of the southward component of B z and the Dst, which for prediction is Dst = (−0.06) + (7.65)B z + t. Some auxiliary conditions should be fulfilled with this, for example the speed of the solar wind should, on average, be on average 350 km s −1 to 750 km s −1 , plasma betaβ should be low and, most importantly, plasma temperature should be low for intense storms.

Metric type-II radio bursts and space weather phenomena: A statistical study

“…• GSs It is well-established that the primary driver of major geomagnetic storms (GSs) (Dungey, 1961) are the ICMEs with southern component on their magnetic field, so-called B z (Richardson and Cane, 2012;Rathore, Gupta, and Kaushik, 2015). Weaker GSs could be also driven by fast streams of solar wind and/or co-rotating or streaming interaction regions (CIRs or SIRs).…”

A substorm-associated enhancement in the XUV radiation measuring channel observed by ESP/EVE/SDO

“…Separate from the magnetic storm, the speed of the solar wind stream goes up to a large value, with a maximum of 670 km s −1 , which is maintained for a rather long time (almost 50 hours or more) with a speed higher than 500 km s −1 . Rathore et al (2015) highlighted the im- portance of solar wind parameters in space weather, two of which were the solar wind speed and the southward component of the Interplanetary Magnetic Field (hereafter IMF).…”

Study of the fractality in a magnetohydrodynamic shell model forced by solar wind fluctuations

“…There are many investigations regarding the relation between interplanetary plasma parameters and the occurrence of geomagnetic events in the Earth's magnetosphere (Kane, 2005;Gonzalez et al, 1994Gonzalez et al, , 2004Tsurutani et al, 1988;Burton et al, 1975;Rathore et al, 2015;Snyder et al, 1963). Among these, Rathore et al (2015) and Kane (2005) show a decrease in the antiparallel geomagnetic field, B s , before the occurrence of the minimum of Dst. While Gonzalez et al (1994Gonzalez et al ( , 2004 and Burton et al (1975) introduce an energy balance equation where the Dst index and the rectified interplanetary electric field (dv • B z ) are related.…”

“…The study of the fractal dimension in various fields has contributed to understanding diverse phenomena, adding a new, interdisciplinary perspective to nonlinear systems. For example, this approach has been used to study seismicity, to describe the distribution of epicenter and hypocenters in a given geographical zone (Pastén et al, 2011), or to consider the relationship between the fractal dimension of the spatial distributions of the aftershocks and the faults (Nanjo and Nagahama, 2004;Sahimi et al, 1993). It has also been used in the study of various catastrophic events such as seismic and epileptic shocks, where the fractality of the relevant time series has been analyzed to extract information on precursor activity (Eftaxias et al, 2006(Eftaxias et al, , 2008.…”