Interplanetary magnetic field control of the location of substorm onset and auroral features in the conjugate hemispheres

Details Interplanetary magnetic field control of the location of substorm onset and auroral features in the conjugate hemispheres Interplanetary magnetic field control of the location of substorm onset and auroral features in the conjugate hemispheres

Jul 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004jgra..10907204o&link_type=abstract

Journal of Geophysical Research, Volume 109, Issue A7, CiteID A07204

Physics

26

Magnetospheric Physics: Magnetospheric Configuration And Dynamics, Magnetospheric Physics: Solar Wind/Magnetosphere Interactions, Magnetospheric Physics: Auroral Phenomena (2407), Magnetospheric Physics: Storms And Substorms, Magnetospheric Physics: Magnetosphere-Inner

Scientific paper

During 2001 and 2002, when the Imager for Magnetopause-to-Aurora Global Exploration (IMAGE) satellite had its apogee in the Northern Hemisphere and the Polar spacecraft, owing to the apsidal precession of its orbit, reached higher altitudes in the Southern Hemisphere, the two spacecraft offered a unique opportunity to study the aurora in the conjugate hemispheres simultaneously. Owing to the large fields of view of the Polar Visible Imaging System (VIS) Earth camera and the IMAGE-FUV instruments, substorms and auroral features were imaged on a global scale in both hemispheres. We have identified five substorm onsets and several auroral features that can be unambiguously identified and compared in the two hemispheres. When mapped onto apex coordinates in the two hemispheres, we find that substorm onset locations and auroral features are usually not symmetric. The longitudinal displacement in one hemisphere compared with the other can be as much as 1.5 hours of local time (~1500 km). For southward interplanetary magnetic field (IMF) the hemispherical asymmetry (ΔMLT) is strongly correlated with the IMF clock angle ($\theta$C) and a linear fit, ΔMLT = -0.017$\theta$C + 3.44, gives a correlation coefficient of 0.83 with a mean deviation of 0.4ΔMLT. These findings are interpreted as the magnetic tensions force acting on open magnetic field lines before reconnecting in the magnetotail. This can also be thought of as the IMF penetrating the magnetosphere.

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