Quasi-Radial IMF Magnetopause PIC 3D Simulations

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Binary file that contains data about solar wind parameters (13 parameters, such as 3D velocity, 3D electric and magnetic fields, density …etc. Data is generated in spherical coordinates. PIC simulation model for radial IMF orientation: the input IMF is only along Sun-Earth line, i.e. cone angle =0.

Binary file that contains data about solar wind parameters (13 parameters, such as 3D velocity, 3D electric and magnetic fields, density …etc. Data is generated in spherical coordinates. PIC simulation model for non-radial IMF orientation: By and Bx is dominant over Bz., i.e. cone angle =50°. This IMF is called in our research paper non-radial IMF.

Binary data that contains the kinetic of backscattering ions (electrons are not included) for solar wind parameters that include density, temperature and velocities for radial IMF.

Binary data that contains the kinetic of backscattering ions (electrons are not included) for solar wind parameters that include density, temperature and velocities for non-radial IMF.

Binary file that contains data about solar wind parameters (13 parameters, such as 3D velocity, 3D electric and magnetic fields, density …etc. Data is generated in cartesian coordinates. PIC simulation model for radial IMF orientation: the input IMF is along Sun-Earth line, i.e. cone angle =0.

Binary file that contains data about solar wind parameters (13 parameters, such as 3D velocity, 3D electric and magnetic fields, density …etc. Data is generated in cartesian coordinates. PIC simulation model for non-radial IMF orientation: By and Bx is dominant over Bz., i.e. cone angle =50°. This IMF is called in our research paper non-radial IMF.

Binary data that contains the ion and electron temperature anisotropy. This file the perpendicular and the parallel components of temperature for both ions and electrons for radial IMF.

Binary data that contains the ion and electron temperature anisotropy. This file the perpendicular and the parallel components of temperature for both ions and electrons for non radial IMF.

The boundary between the solar wind (SW) and the Earths magnetosphere, the magnetopause (MP), is highly dynamic. Its location and shape depend on SW dynamic pressure and interplanetary magnetic field (IMF) orientation. We use a 3D kinetic Particle-In-Cell code (IAPIC) to simulate an event observed by THEMIS spacecraft on July 16, 2007. We investigate the impact of radial (θBx=0◦) and quasi-radial (θBx=50◦) IMF on the shape and size of Earths MP for a dipole tilt of 31◦ using maximum density gradient and pressure balance methods. Using the Shue model as a reference (MP at 10.3 RE), we find that for quasi-radial IMF the MP expands by 1.4 and 1.7RE along the sun-Earth (OX) and tilted magnetic (Tilt) axes, respectively, and it expands by 0.5 and 1.6RE for radial IMF along the same respective axes. When the effect of backstreaming ions is removed from the bulk flow, the expansion ranges are 1.0 and 1.3RE and 0.2, an 1.2RE respectively. It is found that the percentage of backstreaming to bulk flow ions are 16.5%, and 20% for radial and non-radial IMF. We also show that when the backstreaming ions are not resolved, up to 40% of the observed expansion that is due to backstreaming particles can be inadvertently attributed to a change in the SW upstream properties. Finally, we quantified the temperature anisotropy in the magnetosheath, and observe a strong dawn-dusk asymmetry in the MP location.