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Ionospheric Energy Input in Response to Changes in Solar Wind Driving: Statistics From the SuperDARN and AMPERE Campaigns.

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Title: Ionospheric Energy Input in Response to Changes in Solar Wind Driving: Statistics From the SuperDARN and AMPERE Campaigns.
Authors: Billett, D. D.1 (AUTHOR) daniel.billett@usask.ca, McWilliams, K. A.1 (AUTHOR), Perry, G. W.2 (AUTHOR), Clausen, L. B. N.3 (AUTHOR), Anderson, B. J.4 (AUTHOR)
Source: Journal of Geophysical Research. Space Physics. Mar2022, Vol. 127 Issue 3, p1-11. 11p.
Subject Terms: *Geomagnetism, *Upper atmosphere, *Earth currents, Solar wind, Interplanetary magnetic fields, Solar atmosphere
Abstract: For over a decade, the Super Dual Auroral Radar Network and the Active Magnetosphere and Planetary Electrodynamics Response Experiment have been measuring ionospheric convection and field‐aligned currents in the high‐latitude regions, respectively. Using both, high‐latitude maps of the magnetosphere‐ionosphere energy transfer rate (the Poynting flux) have been generated with a time resolution of 2 min between 2010 and 2017. These data driven Poynting flux (PF) patterns are used in this study to perform a superposed epoch analysis of the northern hemisphere ionospheric response to transitions of the interplanetary magnetic field Bz component, upwards of 60° geomagnetic latitude. We discuss the difference in the distribution of PF between the magnetosphere‐ionosphere Dungey cycle "switching on" and "switching off" to solar wind driving, revealing that they are not symmetric temporally or spatially. Plain Language Summary: The Earth's high‐latitude upper atmosphere (the ionosphere, upwards of 100 km in altitude) is consistently bombarded with solar energy that takes the form of electric currents aligned with Earth's magnetic field. The magnetosphere has two generalized states, "open" and "closed." Open is when the Earth and interplanetary magnetic fields (IMFs) connect to each other on the dayside, allowing energy into the atmosphere from the solar wind. Closed is when the fields do not connect (or do not connect simply) and thus not as much energy enters the atmosphere. The aforementioned open or closed states depend on the direction of the IMF, which varies constantly, as well as the history of the field as the magnetosphere takes time to reconfigure. In this study, we utilize nearly 8 years of data to generate average patterns of ionospheric energy input at various intervals before and after the IMF flips in direction. We discuss the spatial and temporal timescales upon which the energy varies in response to the relatively symmetric IMF transitions, finding that they do not result in symmetric changes in the ionospheric energy input patterns. Key Points: The Super Dual Auroral Radar Network and the Active Magnetosphere and Planetary Electrodynamics Response Experiment derived Poynting flux (PF) distributions are used to perform a superposed epoch analysis of interplanetary magnetic field (IMF) Bz transitionsChanges in the IMF Bz component have immediate responses, but continue to evolve for several tens of minutesThere is spatial and temporal asymmetry to how the PF morphology responds to opposite Bz transitions [ABSTRACT FROM AUTHOR]
Copyright of Journal of Geophysical Research. Space Physics is the property of Wiley-Blackwell and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
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  Data: Ionospheric Energy Input in Response to Changes in Solar Wind Driving: Statistics From the SuperDARN and AMPERE Campaigns.
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  Data: <searchLink fieldCode="AR" term="%22Billett%2C+D%2E+D%2E%22">Billett, D. D.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<i> daniel.billett@usask.ca</i><br /><searchLink fieldCode="AR" term="%22McWilliams%2C+K%2E+A%2E%22">McWilliams, K. A.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Perry%2C+G%2E+W%2E%22">Perry, G. W.</searchLink><relatesTo>2</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Clausen%2C+L%2E+B%2E+N%2E%22">Clausen, L. B. N.</searchLink><relatesTo>3</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Anderson%2C+B%2E+J%2E%22">Anderson, B. J.</searchLink><relatesTo>4</relatesTo> (AUTHOR)
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  Data: <searchLink fieldCode="JN" term="%22Journal+of+Geophysical+Research%2E+Space+Physics%22">Journal of Geophysical Research. Space Physics</searchLink>. Mar2022, Vol. 127 Issue 3, p1-11. 11p.
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  Data: For over a decade, the Super Dual Auroral Radar Network and the Active Magnetosphere and Planetary Electrodynamics Response Experiment have been measuring ionospheric convection and field‐aligned currents in the high‐latitude regions, respectively. Using both, high‐latitude maps of the magnetosphere‐ionosphere energy transfer rate (the Poynting flux) have been generated with a time resolution of 2 min between 2010 and 2017. These data driven Poynting flux (PF) patterns are used in this study to perform a superposed epoch analysis of the northern hemisphere ionospheric response to transitions of the interplanetary magnetic field Bz component, upwards of 60° geomagnetic latitude. We discuss the difference in the distribution of PF between the magnetosphere‐ionosphere Dungey cycle "switching on" and "switching off" to solar wind driving, revealing that they are not symmetric temporally or spatially. Plain Language Summary: The Earth's high‐latitude upper atmosphere (the ionosphere, upwards of 100 km in altitude) is consistently bombarded with solar energy that takes the form of electric currents aligned with Earth's magnetic field. The magnetosphere has two generalized states, "open" and "closed." Open is when the Earth and interplanetary magnetic fields (IMFs) connect to each other on the dayside, allowing energy into the atmosphere from the solar wind. Closed is when the fields do not connect (or do not connect simply) and thus not as much energy enters the atmosphere. The aforementioned open or closed states depend on the direction of the IMF, which varies constantly, as well as the history of the field as the magnetosphere takes time to reconfigure. In this study, we utilize nearly 8 years of data to generate average patterns of ionospheric energy input at various intervals before and after the IMF flips in direction. We discuss the spatial and temporal timescales upon which the energy varies in response to the relatively symmetric IMF transitions, finding that they do not result in symmetric changes in the ionospheric energy input patterns. Key Points: The Super Dual Auroral Radar Network and the Active Magnetosphere and Planetary Electrodynamics Response Experiment derived Poynting flux (PF) distributions are used to perform a superposed epoch analysis of interplanetary magnetic field (IMF) Bz transitionsChanges in the IMF Bz component have immediate responses, but continue to evolve for several tens of minutesThere is spatial and temporal asymmetry to how the PF morphology responds to opposite Bz transitions [ABSTRACT FROM AUTHOR]
– Name: AbstractSuppliedCopyright
  Label:
  Group: Ab
  Data: <i>Copyright of Journal of Geophysical Research. Space Physics is the property of Wiley-Blackwell and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
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RecordInfo BibRecord:
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      – Type: doi
        Value: 10.1029/2021JA030102
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      – Code: eng
        Text: English
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      Pagination:
        PageCount: 11
        StartPage: 1
    Subjects:
      – SubjectFull: Geomagnetism
        Type: general
      – SubjectFull: Upper atmosphere
        Type: general
      – SubjectFull: Earth currents
        Type: general
      – SubjectFull: Solar wind
        Type: general
      – SubjectFull: Interplanetary magnetic fields
        Type: general
      – SubjectFull: Solar atmosphere
        Type: general
    Titles:
      – TitleFull: Ionospheric Energy Input in Response to Changes in Solar Wind Driving: Statistics From the SuperDARN and AMPERE Campaigns.
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            NameFull: Billett, D. D.
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            NameFull: Clausen, L. B. N.
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              Text: Mar2022
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              Y: 2022
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