20 Jul Is the Relation Between the Solar power Piece of cake Vibrant Tension plus the Magnetopause Standoff Distance very Easy?

We present results of global magnetohydrodynamic simulations which reconsider the relationship between the solar wind dynamic pressure (P_d) and magnetopause standoff distance (R_Sandwich). We simulate the magnetospheric response to increases in the dynamic pressure hitwe 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 Realization

The newest magnetopause ‘s the line involving the close-Earth area, which is influenced by magnetic profession built in the fresh new Planet’s center, and interplanetary place inhabited from the plasma released about Sunshine known as solar power piece of cake. Within this work, we reexamine the partnership amongst the magnetopause status and parameters out of the fresh solar wind in the shape of computer modeling. It is shown your relationship ranging from solar power wind speed and you can thickness and you will magnetopause standing is more state-of-the-art than just to begin with think.

1 Addition

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 (P_d) 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) B_z component (Aubry et al., 1970 ; Fairfield, 1971 ). A strong southward IMF (B_z<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 P_d and B_z 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.

Recently, Nemecek ainsi que al. ( 2016 ) opposed noticed magnetopause crossings to the Shue et al. model (Shue mais aussi al., 1997 ) to possess half the last solar power course and discovered medical distinctions within design and you will observations. It contended that ionospheric conductivity and solar breeze acceleration was most details one influence the brand new magnetopause reputation. Its statistical analysis suggests that an average magnetopause is farther out-of the world than simply predicted while in the time intervals having lower conductivity and you will highest solar power snap acceleration. They suggested one to intensification out of Ultraviolet rays causes a rise throughout the magnetospheric-ionospheric currents one to reduces the magnetized stress inside magnetosphere and the newest magnetopause actions earthward. Quite the opposite, improvement of your own acceleration intensifies brand new viscous communications involving the solar power snap and you can magnetosphere raising the around the world magnetospheric convection and you will providing more magnetized flux to your dayside magnetosphere. We’re going to talk about such presumptions below about paper.