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Discussion papers | Copyright
https://doi.org/10.5194/angeo-2018-23
© Author(s) 2018. This work is distributed under
the Creative Commons Attribution 4.0 License.

Regular paper 19 Mar 2018

Regular paper | 19 Mar 2018

Review status
This discussion paper is a preprint. It is a manuscript under review for the journal Annales Geophysicae (ANGEO).

Multisatellite observations of the magnetosphere response to changes in the solar wind and interplanetary magnetic field

Galina Korotova1,2, David Sibeck3, Scott Thaller4, John Wygant4, Harlan Spence5, Craig Kletzing6, Vassilis Angelopoulos7, and Robert Redmon8 Galina Korotova et al.
  • 1IPST, University of Maryland, College Park, MD, USA
  • 2IZMIRAN, Russian Academy of Sciences, Moscow, Troitsk, Russia
  • 3Code 674, NASA/GSFC, Greenbelt, MD, USA
  • 4College of Science and Engineering, University of Minnesota, Minneapolis, MN, USA
  • 5EOS, University of New Hampshire, Durham, NH, USA
  • 6Department of Physics and Astronomy, Iowa University, Iowa City, IA, USA
  • 7Department of Earth, Planetary and Space sciences, UCLA, Los Angeles, CA, USA
  • 8Solar and Terrestrial Physics division, NGDC/NOAA, Boulder, CO, USA

Abstract. We employ multipoint observations of the magnetosphere to present case and statistical studies of the electromagnetic field and plasma response to interplanetary (IP) shocks. On February 27, 2014 the initial encounter of an IP shock with the magnetopause occurred on the early postnoon magnetosphere, consistent with the observed alignment of the shock with the spiral IMF. The dayside equatorial magnetosphere exhibited a dusk-dawn oscillatory electrical field with a period of ~330s and peak to peak amplitudes of ~15mV/m for a period of 30min. The intensity of electrons in the energy range from 31.5 to 342KeV responded with periods corresponding to the shock induced ULF electric field waves. The initial electric field perturbation was directed dawnward for this case study. We then perform a statistical study of Ey variations of the electric field and associated plasma drift Vx and Vy flow velocities for 30 magnetospheric events during the passage of interplanetary shocks. The direction of the initial Vx component of plasma flow is tailward at all local times except the nightside magnetosphere, where flows are sunward near the sun-Earth line but antisunward towards dawn and dusk. The observed directions of the azimuthal velocity Vy predominately agree with those expected for the given spiral or orthospiral shock normal orientation.

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Galina Korotova et al.
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We performed case and statistical studies of multipoint observations of the electromagnetic field, plasma and particles in response to an IP shock. We found that the direction of the Vx component of plasma flow is tailward at all local times except the nightside magnetosphere, where flows are sunward near the Sun–Earth line but antisunward towards dawn and dusk.
We performed case and statistical studies of multipoint observations of the electromagnetic...
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