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Is the Family members Involving the Solar power Wind Active Pressure and the Magnetopause Standoff Range thus Quick?
We present results of global magnetohydrodynamic simulations which reconsider the relationship between the solar wind dynamic pressure (Pd) and magnetopause standoff distance (RSandwich). We simulate the magnetospheric response to increases in the dynamic pressure by varying separately the solar wind density or velocity for northward and southward interplanetary magnetic field (IMF). We obtain different values of the power law indices N in the relation depending on which parameter, density, or velocity, has been varied and for which IMF orientation. The changes in the standoff distance are smaller (higher N) for a density increase for southward IMF and greater (smaller N) for a velocity increase.
Basic Words Bottom line
New magnetopause ‘s the line between your near-Earth area, that is influenced because of the magnetized career produced in the brand new Earth’s key, and you may interplanetary room populated of the plasma released on the Sun called the solar snap. Within performs, i reexamine the connection within magnetopause position and you may details away from the fresh new solar power wind in the form of pc acting. It is found that relationship ranging from solar wind acceleration and you can density and magnetopause condition is much more cutting-edge than simply to start with believe.
1 Introduction
The magnetopause is one of principal magnetospheric boundaries which separates dense solar wind plasma in the magnetosheath and tenuous and hot magnetospheric plasma. In response to strong solar wind pressure pulses, the magnetopause comes closer to the Earth and geosynchronous spacecraft may exit the magnetosphere and cross the magnetosheath in the subsolar region or even enter into the supersonic solar wind. To date, more than 15 empirical models of the magnetopause have been developed based on a great number of magnetopause crossings under different solar wind conditions (a list of 14 models published by Suvorova & Dmitriev, 2015 ). Chapman and Ferraro ( 1931 ) suggested that the magnetopause location can be determined from the pressure balance condition between the solar wind dynamic pressure (Pd) and the magnetic pressure of the Earth’s dipole. Besides the dynamic pressure, the second important solar wind parameter influencing the magnetopause position is the interplanetary magnetic field (IMF) Bz component (Aubry et al., 1970 ; Fairfield, 1971 ). A strong southward IMF (Bz<0) results in magnetic reconnection at the dayside magnetopause and intensification of the large-scale field-aligned (Region 1) currents connecting the magnetosphere and ionosphere and moving the magnetopause closer to the Earth (Hill & Rassbach, 1975 ; Sibeck, 1994 ). The Pd and Bz are the only two input parameters in several popular magnetopause models (e.g., Petrinec & Russell, 1996 ; Roelof & Sibeck, 1993 ; Shue et al., 1997 ; 1998 ; Sibeck et al., 1991 ). The recent (Lin et al., 2010 ) empirical model replaces the solar wind dynamic pressure by the sum of dynamic and magnetic pressures and takes into account the Earth’s dipole tilt. Moreover, several papers (Dusik et al., 2010 ; Grygorov et al., 2017 ; Merka et al., 2003 ; Samso ) note that the magnetopause significantly expands during radial IMF intervals concluding that the IMF cone angle (the angle between IMF and the Sun-Earth line) eter for calculation of the magnetopause location.
Has just, Nemecek ainsi que al. ( 2016 ) opposed seen magnetopause crossings into the Shue mais aussi al. design (Shue mais aussi al., 1997 ) getting half the very last solar power course and discovered medical variations involving the design and you can observations. It debated that ionospheric conductivity https://datingranking.net/pl/mexican-cupid-recenzja/ as well as the solar wind velocity is even more details one to determine the new magnetopause position. The analytical studies shows that the average magnetopause was farther off our planet than forecast throughout the date durations which have lower conductivity and you can higher solar snap speed. They recommended that intensification from Ultraviolet radiation contributes to a growth in the magnetospheric-ionospheric currents that decreases the magnetized pressure in the magnetosphere and you will new magnetopause motions earthward. On the other hand, improvement of one’s speed intensifies new viscous telecommunications between the solar piece of cake and you can magnetosphere improving the globally magnetospheric convection and you will getting a lot more magnetic flux with the dayside magnetosphere. We will mention this type of assumptions less than on the paper.
