International Journal of Astrophysics and Space Science

| Peer-Reviewed |

Effects of Geomagnetic Storm on Ionospheric TEC Variability over High Latitude Regions

Received: 24 June 2022    Accepted: 26 July 2022    Published: 10 August 2022
Views:       Downloads:

Share This Article

Abstract

The effects of the geomagnetic storm on August 26, 2018 on the ionospheric TEC fluctuations in the high latitude region were investigated. This study is based on TEC data obtained by the UNAVCO dual-frequency GPS devices at the northern stations of Hofn and Kiruna, and the southern stations of Mawson and Syog. The results of this study show that the variation of TEC is more noticeable in the northern hemisphere of the Hofn and Kiruna stations than in the southern hemisphere of the Mawson and Syog stations on the August 26, 2018 storm. Interestingly, the midnight TEC became comparable to the daytime TEC over both northern and southern stations, indicating the ingestion of additional plasma from higher latitudes into the northern stations. The positive enhancement of ∆TEC values were higher over Hofn and Kiruna on August 26, 2018 by about 170%, and 180% than Mawson and Syog by about 70%, and 150% stations, respectively. During geomagnetic storm of August 26, 2018, the Hofn and Kiruna stations had a much greater negative impact on ∆TEC = -50% than the Mawson and Syog stations ∆TEC = -40%. The ∆TEC over each station are caused by a significant rise in the Kp index and the opposite polarity of the interplanetary electric field (IEF Ey) in the northward direction and the southward decrease of the interplanetary magnetic field (IMF Bz). The decrease in Dst-index and ∆H during the main phase of the storm increased TEC over Kiruna and Mawson stations. Furthermore, the values of changes in TEC was stronger over Kiruna station in the northern hemisphere than over Mawson station in the southern hemisphere, indicating that the northern stations received more additional plasma than the southern stations during the August 26, 2018 geomagnetic storm. During the August 26, 2018 geomagnetic storm, the values of the horizontal component of Earth’s magnetic field decreased more over Kiruna station, about ∆H = -1500 nT, than over Mawson station, about ∆H = -1300 nT. As a result, the changes in TEC are more pronounced over Kiruna station, where ∆TEC = 180%, than over Mawson station, where ∆TEC = 70%. This indicates that during the August 26, 2018 geomagnetic storm, the northern hemisphere receives more energy from the solar wind, which produces particle acceleration and precipitation, higher field aligned currents, and ionospheric electrojets.

DOI 10.11648/j.ijass.20221002.11
Published in International Journal of Astrophysics and Space Science (Volume 10, Issue 2, June 2022)
Page(s) 18-27
Creative Commons

This is an Open Access article, distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution and reproduction in any medium or format, provided the original work is properly cited.

Copyright

Copyright © The Author(s), 2024. Published by Science Publishing Group

Keywords

Ionospheric TEC, Geomagnetic Storm, TEC Enhancement, TEC Variability

References
[1] F. D’ujanga, P. Baki, J. Olwendo, and B. Twinamasiko, “Total electron content of the ionosphere at two stations in east africa during the 24–25 october 2011 geomagnetic storm,” Advances in Space Research, vol. 51, no. 5, pp. 712–721, 2013.
[2] E. A. Ariyibi, E. O. Joshua, and B. A. Rabiu, “Studies of ionospheric variations during geomagnetic activities at the low-latitude station, ile-ife, nigeria,” Acta Geophysica, vol. 61, no. 1, pp. 223–239, 2013.
[3] R. S. Fayose, R. Babatunde, O. Oladosu, and K. Groves, “Variation of total electron content [tec] and their effect on gnss over akure, nigeria,” Applied Physics Research, vol. 4, no. 2, p. 105, 2012.
[4] A. Jain, S. Tiwari, S. Jain, and A. Gwal, “Tec response during severe geomagnetic storms near the crest of equatorial ionization anomaly,” 94.20. Vv; 94.30. Lr, 2010.
[5] W. D. Gonzalez, B. T. Tsurutani, and A. L. Clúa de Gonzalez, “Interplanetaryoriginofgeomagneticstorms,” Space Science Reviews, vol. 88, no. 3, pp. 529–562, 1999.
[6] C. Russell, “The solar wind interaction with the earth’s magnetosphere: A tutorial,” IEEE transactions on plasma science, vol. 28, no. 6, pp. 1818–1830, 2000.
[7] W. H. Campbell, “Geomagnetic storms, the dst ring- current myth and lognormal distributions,” Journal of Atmospheric and Terrestrial Physics, vol. 58, no. 10, pp. 1171–1187, 1996.
[8] B. T. Tsurutani, G. S. Lakhina, and R. Hajra, “The physics of space weather/solar-terrestrial physics (stp): what we know now and what the current and future challenges are,” Nonlinear Processes in Geophysics, vol. 27, no. 1, pp. 75–119, 2020.
[9] L. J. Paxton, Y. Zhang, H. Kil, and R. K. Schaefer, “Exploring the upper atmosphere: Using optical remote sensing,” Upper Atmosphere Dynamics and Energetics, pp. 487–522, 2021.
[10] C.-C. Wu and R. Lepping, “Effects of magnetic clouds on the occurrence of geomagnetic storms: The first 4 years of wind,” Journal of Geophysical Research: Space Physics, vol. 107, no. A10, pp. SMP–19, 2002.
[11] S. Basu, S. Basu, C. Valladares, H.-C. Yeh, S.-Y. Su, E. MacKenzie, P. Sultan, J. Aarons, F. Rich, P. Doherty, et al., “Ionospheric effects of major magnetic storms during the international space weather period of september and october 1999: Gps observations, vhf/uhf scintillations, and in situ density structures at middle and equatorial latitudes,” Journal of Geophysical Research: Space Physics, vol. 106, no. A12, pp. 30389–30413, 2001.
[12] H. U. Frey, “Localized aurora beyond the auroral oval,” Reviews of Geophysics, vol. 45, no. 1, 2007.
[13] A. Richmond and G. Lu, “Upper-atmospheric effects of magnetic storms: a brief tutorial,” Journal of Atmospheric and Solar-Terrestrial Physics, vol. 62, no. 12, pp. 1115–1127, 2000.
[14] P. Khatarkar, P. Bhawre, V. Kachneria, P. Purohit, and A. Gwal, “Behavior of total electron content over auroral region at maitri, antarctica,” International Journal of Scientific & Engineering Research, vol. 5, no. 9, pp. 1–7, 2014.
[15] M. Abdu, “Equatorial ionosphere–thermosphere system: Electrodynamics and irregularities,” Advances in Space Research, vol. 35, no. 5, pp. 771–787, 2005.
[16] P. R. Fagundes, F. Cardoso, B. Fejer, K. Venkatesh, B. Ribeiro, and V. Pillat, “Positive and negative gps- tec ionospheric storm effects during the extreme space weather event of march 2015 over the brazilian sector,” Journal of Geophysical Research: Space Physics, vol. 121, no. 6, pp. 5613–5625, 2016.
[17] W. Wang, J. Lei, A. G. Burns, S. C. Solomon, M. Wiltberger, J. Xu, Y. Zhang, L. Paxton, and A. Coster, “Ionospheric response to the initial phase of geomagnetic storms: Common features,” Journal of Geophysical Research: Space Physics, vol. 115, no. A7, 2010.
[18] B. Tsurutani, A. Mannucci, B. Iijima, M. A. Abdu, J. H. A. Sobral, W. Gonzalez, F. Guarnieri, T. Tsuda, A. Saito, K. Yumoto, et al., “Global dayside ionospheric uplift and enhancement associated with interplanetary electric fields,” Journal of Geophysical Research: Space Physics, vol. 109, no. A8, 2004.
[19] S. Basu, E. MacKenzie, S. Basu, H. Carlson, D. Hardy, F. Rich, and R. Livingston, “Coordinated measurements of low-energy electron precipitation and scintillations/tec in the auroral oval,” Radio science, vol. 18, no. 6, pp. 1151–1165, 1983.
[20] R. Dabas, P. Bhuyan, T. Tyagi, R. Bhardwaj, and J. Lal, “Day-to-day changes in ionospheric electron content at low latitudes,” Radio science, vol. 19, no. 03, pp. 749– 756, 1984.
[21] P. Doherty, E. Raffi, J. Klobuchar, and M. B. El-Arini, “Statistics of time rate of change of ionospheric range delay,” in Proceedings of ION GPS-94, part, vol. 2, 1994.
[22] E. Astafyeva, Y. Yasyukevich, A. Yasyukevich, B. Maletckii, and S. Syrovatskii, “High-latitude ionospheric irregularities during the 25–26 august 2018 geomagnetic storm as seen by ground-based and space- borne instruments,” in 2021 XXXIVth General Assembly and Scientific Symposium of the International Union of Radio Science (URSI GASS), pp. 1–4, IEEE, 2021.
[23] D. Blagoveshchensky and M. Sergeeva, “Ionospheric parameters in the european sector during the magnetic storm of august 25–26, 2018,” Advances in Space Research, vol. 65, no. 1, pp. 11–18, 2020.
[24] G. A. Mansilla, “Behavior of the total electron content over the arctic and antarctic sectors during several intense geomagnetic storms,” Geodesy and Geodynamics, vol. 10, no. 1, pp. 26–36, 2019.
[25] O. Bolaji, J. Fashae, S. Adebiyi, C. Owolabi, B. Adebesin, R. Kaka, J. Ibanga, M. Abass, O. Akinola, B. Adekoya, et al., “Storm time effects on latitudinal distribution of ionospheric tec in the american and asian- australian sectors: August 25–26, 2018 geomagnetic storm,” Journal of Geophysical Research: Space Physics, vol. 126, no. 8, p. e2020JA029068, 2021.
[26] A. Van Dierendonck, J. Klobuchar, and Q. Hua, “Ionospheric scintillation monitoring using commercial single frequency c/a code receivers,” in proceedings of ION GPS, vol. 93, pp. 1333–1342, 1993.
[27] I. Cherniak and I. Zakharenkova, “Large-scale traveling ionospheric disturbances origin and propagation: Case study of the december 2015 geomagnetic storm,” Space Weather, vol. 16, no. 9, pp. 1377–1395, 2018.
[28] I. Cherniak and I. Zakharenkova, “High-latitude ionospheric irregularities: differences between ground- and space-based gps measurements during the 2015 st. patrick’s day storm,” Earth, Planets and Space, vol. 68, no. 1, pp. 1–13, 2016.
[29] A. O. Olabode and E. A. Ariyibi, “Geomagnetic storm main phase effect on the equatorial ionosphere over ile–ife as measured from gps observations,” Scientific African, vol. 9, p. e00472, 2020.
[30] C. S. Carrano and K. M. Groves, “The gps segment of the afrl-scinda global network and the challenges of real-time tec estimation in the equatorial ionosphere,” in Proceedings of the 2006 National Technical Meeting of The Institute of Navigation, pp. 1036–1047, 2006.
[31] C. U. Idosa and K. S. Rikitu, “Effects of total solar eclipse on ionospheric total electron content over antarctica on 2021 december 4,” The Astrophysical Journal, vol. 932, no. 1, p. 2, 2022.
[32] V. A. Eyelade, A. O. Adewale, A. O. akala, O. S. Bolaji, and A. B. Rabiu, “Studying the variability in the diurnal and seasonal variations in gps total electron content over nigeria,” in Annales Geophysicae, vol. 35, pp. 701–710, Copernicus GmbH, 2017.
[33] J. Lean, R. Meier, J. Picone, and J. Emmert, “Ionospheric total electron content: Global and hemispheric climatology,” Journal of Geophysical Research: Space Physics, vol. 116, no. A10, 2011.
[34] P. Bhuyan and R. R. Borah, “Tec derived from gps network in india and comparison with the iri,” Advances in Space Research, vol. 39, no. 5, pp. 830–840, 2007.
[35] O. Verkhoglyadova, B. Tsurutani, A. Mannucci, M. Mlynczak, L. Hunt, L. Paxton, and A. Komjathy, “Solar wind driving of ionosphere-thermosphere responses in three storms near st. patrick’s day in 2012, 2013, and 2015,” Journal of Geophysical Research: Space Physics, vol. 121, no. 9, pp. 8900–8923, 2016.
[36] T. Yeeram, “Interplanetary drivers of daytime penetration electric field into equatorial ionosphere during cir- induced geomagnetic storms,” Journal of Atmospheric and Solar-Terrestrial Physics, vol. 157, pp. 6–15, 2017.
[37] B. Adhikari, S. Dahal, and N. P. Chapagain, “Study of field-aligned current (fac), interplanetary electric field component (ey), interplanetary magnetic field component (bz), and northward (x) and eastward (y) components of geomagnetic field during supersubstorm,” Earth and Space Science, vol. 4, no. 5, pp. 257–274, 2017.
[38] I. A. Daglis, R. M. Thorne, W. Baumjohann, and S. Orsini, “The terrestrial ring current: Origin, formation, and decay,” Reviews of Geophysics, vol. 37, no. 4, pp. 407–438, 1999.
[39] L. Juusola et al., “Observations of the solar wind- magnetosphere-ionosphere coupling,” 2009.
[40] R. W. Schunk, P. M. Banks, and W. J. Raitt, “Effects of electric fields and other processes upon the nighttime high-latitude f layer,” Journal of Geophysical Research, vol. 81, no. 19, pp. 3271–3282, 1976.
[41] B. Adhikari, B. Kaphle, N. Adhikari, S. Limbu, A. Sunar, R. K. Mishra, and S. Adhikari, “Analysis of cosmic ray, solar wind energies, components of earth’s magnetic field, and ionospheric total electron content during solar superstorm of november 18–22, 2003,” SN Applied Sciences, vol. 1, no. 5, pp. 1–10, 2019.
[42] I. Shagimuratov, A. Krankowski, I. Ephishov, Y. Cherniak, P. Wielgosz, and I. Zakharenkova, “High latitude tec fluctuations and irregularity oval during geomagnetic storms,” Earth, planets and space, vol. 64, no. 6, pp. 521–529, 2012.
Cite This Article
  • APA Style

    Chali Idosa Uga. (2022). Effects of Geomagnetic Storm on Ionospheric TEC Variability over High Latitude Regions. International Journal of Astrophysics and Space Science, 10(2), 18-27. https://doi.org/10.11648/j.ijass.20221002.11

    Copy | Download

    ACS Style

    Chali Idosa Uga. Effects of Geomagnetic Storm on Ionospheric TEC Variability over High Latitude Regions. Int. J. Astrophys. Space Sci. 2022, 10(2), 18-27. doi: 10.11648/j.ijass.20221002.11

    Copy | Download

    AMA Style

    Chali Idosa Uga. Effects of Geomagnetic Storm on Ionospheric TEC Variability over High Latitude Regions. Int J Astrophys Space Sci. 2022;10(2):18-27. doi: 10.11648/j.ijass.20221002.11

    Copy | Download

  • @article{10.11648/j.ijass.20221002.11,
      author = {Chali Idosa Uga},
      title = {Effects of Geomagnetic Storm on Ionospheric TEC Variability over High Latitude Regions},
      journal = {International Journal of Astrophysics and Space Science},
      volume = {10},
      number = {2},
      pages = {18-27},
      doi = {10.11648/j.ijass.20221002.11},
      url = {https://doi.org/10.11648/j.ijass.20221002.11},
      eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ijass.20221002.11},
      abstract = {The effects of the geomagnetic storm on August 26, 2018 on the ionospheric TEC fluctuations in the high latitude region were investigated. This study is based on TEC data obtained by the UNAVCO dual-frequency GPS devices at the northern stations of Hofn and Kiruna, and the southern stations of Mawson and Syog. The results of this study show that the variation of TEC is more noticeable in the northern hemisphere of the Hofn and Kiruna stations than in the southern hemisphere of the Mawson and Syog stations on the August 26, 2018 storm. Interestingly, the midnight TEC became comparable to the daytime TEC over both northern and southern stations, indicating the ingestion of additional plasma from higher latitudes into the northern stations. The positive enhancement of ∆TEC values were higher over Hofn and Kiruna on August 26, 2018 by about 170%, and 180% than Mawson and Syog by about 70%, and 150% stations, respectively. During geomagnetic storm of August 26, 2018, the Hofn and Kiruna stations had a much greater negative impact on ∆TEC = -50% than the Mawson and Syog stations ∆TEC = -40%. The ∆TEC over each station are caused by a significant rise in the Kp index and the opposite polarity of the interplanetary electric field (IEF Ey) in the northward direction and the southward decrease of the interplanetary magnetic field (IMF Bz). The decrease in Dst-index and ∆H during the main phase of the storm increased TEC over Kiruna and Mawson stations. Furthermore, the values of changes in TEC was stronger over Kiruna station in the northern hemisphere than over Mawson station in the southern hemisphere, indicating that the northern stations received more additional plasma than the southern stations during the August 26, 2018 geomagnetic storm. During the August 26, 2018 geomagnetic storm, the values of the horizontal component of Earth’s magnetic field decreased more over Kiruna station, about ∆H = -1500 nT, than over Mawson station, about ∆H = -1300 nT. As a result, the changes in TEC are more pronounced over Kiruna station, where ∆TEC = 180%, than over Mawson station, where ∆TEC = 70%. This indicates that during the August 26, 2018 geomagnetic storm, the northern hemisphere receives more energy from the solar wind, which produces particle acceleration and precipitation, higher field aligned currents, and ionospheric electrojets.},
     year = {2022}
    }
    

    Copy | Download

  • TY  - JOUR
    T1  - Effects of Geomagnetic Storm on Ionospheric TEC Variability over High Latitude Regions
    AU  - Chali Idosa Uga
    Y1  - 2022/08/10
    PY  - 2022
    N1  - https://doi.org/10.11648/j.ijass.20221002.11
    DO  - 10.11648/j.ijass.20221002.11
    T2  - International Journal of Astrophysics and Space Science
    JF  - International Journal of Astrophysics and Space Science
    JO  - International Journal of Astrophysics and Space Science
    SP  - 18
    EP  - 27
    PB  - Science Publishing Group
    SN  - 2376-7022
    UR  - https://doi.org/10.11648/j.ijass.20221002.11
    AB  - The effects of the geomagnetic storm on August 26, 2018 on the ionospheric TEC fluctuations in the high latitude region were investigated. This study is based on TEC data obtained by the UNAVCO dual-frequency GPS devices at the northern stations of Hofn and Kiruna, and the southern stations of Mawson and Syog. The results of this study show that the variation of TEC is more noticeable in the northern hemisphere of the Hofn and Kiruna stations than in the southern hemisphere of the Mawson and Syog stations on the August 26, 2018 storm. Interestingly, the midnight TEC became comparable to the daytime TEC over both northern and southern stations, indicating the ingestion of additional plasma from higher latitudes into the northern stations. The positive enhancement of ∆TEC values were higher over Hofn and Kiruna on August 26, 2018 by about 170%, and 180% than Mawson and Syog by about 70%, and 150% stations, respectively. During geomagnetic storm of August 26, 2018, the Hofn and Kiruna stations had a much greater negative impact on ∆TEC = -50% than the Mawson and Syog stations ∆TEC = -40%. The ∆TEC over each station are caused by a significant rise in the Kp index and the opposite polarity of the interplanetary electric field (IEF Ey) in the northward direction and the southward decrease of the interplanetary magnetic field (IMF Bz). The decrease in Dst-index and ∆H during the main phase of the storm increased TEC over Kiruna and Mawson stations. Furthermore, the values of changes in TEC was stronger over Kiruna station in the northern hemisphere than over Mawson station in the southern hemisphere, indicating that the northern stations received more additional plasma than the southern stations during the August 26, 2018 geomagnetic storm. During the August 26, 2018 geomagnetic storm, the values of the horizontal component of Earth’s magnetic field decreased more over Kiruna station, about ∆H = -1500 nT, than over Mawson station, about ∆H = -1300 nT. As a result, the changes in TEC are more pronounced over Kiruna station, where ∆TEC = 180%, than over Mawson station, where ∆TEC = 70%. This indicates that during the August 26, 2018 geomagnetic storm, the northern hemisphere receives more energy from the solar wind, which produces particle acceleration and precipitation, higher field aligned currents, and ionospheric electrojets.
    VL  - 10
    IS  - 2
    ER  - 

    Copy | Download

Author Information
  • Department of Physics, Faculty of Natural Science, Jimma University, Jimma, Ethiopia

  • Sections