The Growth of Ring Current/SYM‐H Under Northward IMF Bz Conditions Present During the 21–22 January 2005 Geomagnetic Storm
Abstract The total energy transfer from the solar wind to the magnetosphere is governed by the reconnection rate at the magnetosphere edges as the Z‐component of interplanetary magnetic field (IMF Bz) turns southward. The geomagnetic storm on 21–22 January 2005 is considered to be anomalous as the S...
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Wiley
2023-10-01
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| Series: | Space Weather |
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| Online Access: | https://doi.org/10.1029/2023SW003489 |
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| author | Diptiranjan Rout S. Patra S. Kumar D. Chakrabarty G. D. Reeves C. Stolle K. Pandey S. Chakraborty E. A. Spencer |
| author_facet | Diptiranjan Rout S. Patra S. Kumar D. Chakrabarty G. D. Reeves C. Stolle K. Pandey S. Chakraborty E. A. Spencer |
| author_sort | Diptiranjan Rout |
| collection | DOAJ |
| description | Abstract The total energy transfer from the solar wind to the magnetosphere is governed by the reconnection rate at the magnetosphere edges as the Z‐component of interplanetary magnetic field (IMF Bz) turns southward. The geomagnetic storm on 21–22 January 2005 is considered to be anomalous as the SYM‐H index that signifies the strength of ring current, decreases and had a sustained trough value of −101 nT lasting more than 6 hr under northward IMF Bz conditions. In this work, the standard WINDMI model is utilized to estimate the growth and decay of magnetospheric currents by using several solar wind‐magnetosphere coupling functions. However, it is found that the WINDMI model driven by any of these coupling functions is not fully able to explain the decrease of SYM‐H under northward IMF Bz. A dense plasma sheet along with signatures of a highly stretched magnetosphere was observed during this storm. The SYM‐H variations during the entire duration of the storm were only reproduced after modifying the WINDMI model to account for the effects of the dense plasma sheet. The limitations of directly driven models relying purely on the solar wind parameters and not accounting for the state of the magnetosphere are highlighted by this work. |
| format | Article |
| id | doaj-art-ba64d760e7cc4585bf704d3dbb5939c2 |
| institution | Kabale University |
| issn | 1542-7390 |
| language | English |
| publishDate | 2023-10-01 |
| publisher | Wiley |
| record_format | Article |
| series | Space Weather |
| spelling | doaj-art-ba64d760e7cc4585bf704d3dbb5939c22025-01-14T16:31:16ZengWileySpace Weather1542-73902023-10-012110n/an/a10.1029/2023SW003489The Growth of Ring Current/SYM‐H Under Northward IMF Bz Conditions Present During the 21–22 January 2005 Geomagnetic StormDiptiranjan Rout0S. Patra1S. Kumar2D. Chakrabarty3G. D. Reeves4C. Stolle5K. Pandey6S. Chakraborty7E. A. Spencer8GFZ German Research Centre for Geosciences Potsdam GermanyUniversity of New Brunswick Fredericton NB CanadaInstitute for Space‐Earth Environmental Research Nagoya University Nagoya JapanPhysical Research Laboratory Ahmedabad IndiaLos Alamos National Laboratory Los Alamos NM USALeibniz Institute of Atmospheric Physics at the University of Rostock Kuhlüngsborn GermanyDepartment of Physics and Engineering Physics ISAS University of Saskatchewan Saskatoon SK CanadaCenter for Space Science and Engineering Research Bradley Department of Electrical and Computer Engineering Virginia Tech Blacksburg VA USADepartment of Electrical and Computer Engineering University of South Alabama Mobile AL USAAbstract The total energy transfer from the solar wind to the magnetosphere is governed by the reconnection rate at the magnetosphere edges as the Z‐component of interplanetary magnetic field (IMF Bz) turns southward. The geomagnetic storm on 21–22 January 2005 is considered to be anomalous as the SYM‐H index that signifies the strength of ring current, decreases and had a sustained trough value of −101 nT lasting more than 6 hr under northward IMF Bz conditions. In this work, the standard WINDMI model is utilized to estimate the growth and decay of magnetospheric currents by using several solar wind‐magnetosphere coupling functions. However, it is found that the WINDMI model driven by any of these coupling functions is not fully able to explain the decrease of SYM‐H under northward IMF Bz. A dense plasma sheet along with signatures of a highly stretched magnetosphere was observed during this storm. The SYM‐H variations during the entire duration of the storm were only reproduced after modifying the WINDMI model to account for the effects of the dense plasma sheet. The limitations of directly driven models relying purely on the solar wind parameters and not accounting for the state of the magnetosphere are highlighted by this work.https://doi.org/10.1029/2023SW003489ring currentspace weathernorthward IMF BzWINDMI modelsolar wind‐magnetosphere‐ionosphere coupling |
| spellingShingle | Diptiranjan Rout S. Patra S. Kumar D. Chakrabarty G. D. Reeves C. Stolle K. Pandey S. Chakraborty E. A. Spencer The Growth of Ring Current/SYM‐H Under Northward IMF Bz Conditions Present During the 21–22 January 2005 Geomagnetic Storm Space Weather ring current space weather northward IMF Bz WINDMI model solar wind‐magnetosphere‐ionosphere coupling |
| title | The Growth of Ring Current/SYM‐H Under Northward IMF Bz Conditions Present During the 21–22 January 2005 Geomagnetic Storm |
| title_full | The Growth of Ring Current/SYM‐H Under Northward IMF Bz Conditions Present During the 21–22 January 2005 Geomagnetic Storm |
| title_fullStr | The Growth of Ring Current/SYM‐H Under Northward IMF Bz Conditions Present During the 21–22 January 2005 Geomagnetic Storm |
| title_full_unstemmed | The Growth of Ring Current/SYM‐H Under Northward IMF Bz Conditions Present During the 21–22 January 2005 Geomagnetic Storm |
| title_short | The Growth of Ring Current/SYM‐H Under Northward IMF Bz Conditions Present During the 21–22 January 2005 Geomagnetic Storm |
| title_sort | growth of ring current sym h under northward imf bz conditions present during the 21 22 january 2005 geomagnetic storm |
| topic | ring current space weather northward IMF Bz WINDMI model solar wind‐magnetosphere‐ionosphere coupling |
| url | https://doi.org/10.1029/2023SW003489 |
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