Articles | Volume 40, issue 6
https://doi.org/10.5194/angeo-40-619-2022
© Author(s) 2022. This work is distributed under
the Creative Commons Attribution 4.0 License.
the Creative Commons Attribution 4.0 License.
https://doi.org/10.5194/angeo-40-619-2022
© Author(s) 2022. This work is distributed under
the Creative Commons Attribution 4.0 License.
the Creative Commons Attribution 4.0 License.
Regular paper
| 
02 Nov 2022
Regular paper |
| 02 Nov 2022
| 02 Nov 2022
Multi-instrument observations of polar cap patches and traveling ionospheric disturbances generated by solar wind Alfvén waves coupling to the dayside magnetosphere
Physics Department, University of New Brunswick,
Fredericton, NB, E3B 5A3, Canada
Robert G. Gillies
Department of Physics and Astronomy, University of
Calgary, Calgary, AB, Canada
David R. Themens
Physics Department, University of New Brunswick,
Fredericton, NB, E3B 5A3, Canada
School of Engineering, University of Birmingham,
Birmingham, UK
James M. Weygand
Earth, Planetary, and Space Sciences, University of
California, Los Angeles, CA, USA
Evan G. Thomas
Thayer School of Engineering, Dartmouth College, Hanover,
NH, USA
Shibaji Chakraborty
Bradley Department of Electrical and Computer Engineering,
Virginia Tech, Blacksburg, VA, USA
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Subject: Earth's ionosphere & aeronomy | Keywords: Ionosphere–magnetosphere interactions
Ionospheric upwelling and the level of associated noise at solar minimum
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Whistler waves produced by monochromatic currents in the low nighttime ionosphere
Ionospheric control of space weather
Swarm field-aligned currents during a severe magnetic storm of September 2017
Timothy Wemimo David, Chizurumoke Michael Michael, Darren Wright, Adetoro Temitope Talabi, and Abayomi Ekundayo Ajetunmobi
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The Earth’s upper atmospheres are dominated by matter also known as plasma. These plasmas can flow from the lower region, the ionosphere, to the further-up region, the magnetosphere, which is described as upwelling. We analyse data for ionospheric upwelling over the solar minimum period. A main finding is that the noise or rejected data in the dataset were predominant around the local evening and in winter and minimum around local noon and in summer.
Liisa Juusola, Ari Viljanen, Noora Partamies, Heikki Vanhamäki, Mirjam Kellinsalmi, and Simon Walker
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Osuke Saka
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Transverse electric fields transmitted from the magnetosphere and those generated by the neutral winds yield a local breakdown of the charge neutrality at the boundaries between the thermosphere and mesosphere. The breakdown may create parallel electric fields in the thermosphere to produce spiral auroras and outflows. This explanation supposes an auroral generator located not in a distant space, but rather in our much nearer upper atmosphere.
Andrew J. Mazzella Jr. and Endawoke Yizengaw
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Ângela M. Santos, Christiano G. M. Brum, Inez S. Batista, José H. A. Sobral, Mangalathayil A. Abdu, and Jonas R. Souza
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Osuke Saka
Ann. Geophys., 39, 455–460, https://doi.org/10.5194/angeo-39-455-2021, https://doi.org/10.5194/angeo-39-455-2021, 2021
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During the most intense storm of solar cycle 24, the magnetosphere–ionosphere interaction, which is primarily associated with field-aligned currents (FACs), was much stronger than usual. Measurements onboard the low-latitude polar-orbiting Swarm satellites have shown that the intensities of FACs increase dramatically during the storm-time substorms. The extreme values of 1 s (7.5 km width) FACs reach 80 μA m−2. The lowest latitude of the FAC region is limited to 49–50 MLat.
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Short summary
The solar wind interaction with Earth’s magnetic field deposits energy into the upper portion of the atmosphere at high latitudes. The coupling process that modulates the ionospheric convection and intensity of ionospheric currents leads to formation of densely ionized patches convecting across the polar cap. The ionospheric currents launch traveling ionospheric disturbances (TIDs) propagating equatorward. The polar cap patches and TIDs are then observed by networks of radars and GPS receivers.
The solar wind interaction with Earth’s magnetic field deposits energy into the upper portion...
