Coupled Evolution of Storm-Enhanced Density, Tongue of Ionization, and Polar Ionospheric Hole during the 10 May 2024 Superstorm

ZHANG Shun-Rong; COSTER Anthea J; Ercha AA; THAYYIL Jayachandran P; ZHANG Yongliang

doi:10.11728/cjss2026.05.2026-0019

Coupled Evolution of Storm-Enhanced Density, Tongue of Ionization, and Polar Ionospheric Hole during the 10 May 2024 Superstorm

doi: 10.11728/cjss2026.05.2026-0019 cstr: 32142.14.cjss.2026-0019

1.
Haystack Observatory, Massachusetts Institute of Technology, Westford, MA 01886
2.
Physics Department, University of New Brunswick, Fredericton, NB E3B 5A3
3.
Applied Physics Lab, Johns Hopkins University, Laurel, MD 20723

More Information

Author Bio:
Dr. Shun-Rong Zhang, the first author and corresponding author, is a Principal Research Scientist at MIT Haystack Observatory. He has been actively involved in a diverse range of ionosphere and upper atmosphere research, encompassing geospace storm effects, variability, climatology, long-term changes, and the associated coupling processes in ionosphere-thermosphere-magnetosphere and atmospheric systems. E-mail: shunrong@mit.edu

摘要

Abstract: This study investigates the concurrent evolution of subauroral storm-enhanced density (SED), the polar Tongue Of Ionization (TOI), and the Polar Ionospheric Hole (PIH) during the 10 May 2024 geomagnetic superstorm. Using global GNSS Total Electron Content (TEC) and TIMED/GUVI thermospheric O/N₂ ratio measurements, we focus on the interplay between ionized and neutral density structures at polar latitudes. Our observation exhibited the following scenario that highlights the new understanding of peculiar O/N₂ influences on TOI and plasma patches during this storm. (i) With the arrival of the ICME shock and subsequent Interplanetary Magnetic Field (IMF) B_z southward turning, Prompt Penetration Electric Field (PPEF) drove Equatorial Ionization Anomaly (EIA) crests moving poleward, causing a mid-latitude density enhancement. At midlatitude, the poleward Subauroral Polarization Stream (SAPS) provided significantly intensified sunward flow, while PPEF generated poleward flow, thus the two ion drift components led to the buildup of high electron density, forming the SED base and plume. (ii) At noon, the SED plume was entrained into the anti-sunward flow channel toward the polar cap. (iii) An unusual dayside PIH was formed as the neutral gas with a depleted O/N₂ ratio began circulating in the morning sector toward afternoon. This presumed neutral circulation was primarily driven by the increased ion drag associated with significant storm-time auroral electric fields. (iv) Fresh TOI plasma is moving into the polar cap and rotating eastward, with some portion continuing antisunward convecting. Successively following the TOI eastward convection, the PIH also rotates eastward. (v) PIH and TOI continued to be depleted, with TOI being segmented, as the entire polar cap was soaked by the substantially suppressed O/N₂ air. The TOI and PIH remained eastward convicting for several hours, including a 2-hour interval of larger positive IMF B_y.
- Tongue of ionization /
- Storm-enhanced density /
- Plasma patches /
- Thermospheric composition (O/N₂) /
- Magnetosphere-ionosphere-thermosphere coupling /
- Geomagnetic storms
注释:
Conflict of Interests:

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Figure 1. Solar geophysical conditions for 10–12 May 2024. IMF B_y and B_z (a), interplanetary electric field (b), SYM-H index (c), solar wind dynamic pressure (d), auroral AU and AL index (e)

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Figure 2. Latitudinal and UT variations in TEC (TECU, a and d), TEC relative changes (percentage fraction) from the reference on 10 May 2024 (b and e), and dTEC (TECU, c and f) in American (left panels) and Asian (right panels) sectors which have 12-hour local time offset. Dashed lines mark the ICME arrival induced simultaneous ionospheric variations

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Figure 3. A sequence of global TEC maps to demonstrate the SED development. TEC variations are shown as absolute difference from the reference day 10 May 2024 (left) and relative percentage (fractional) change (right)

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Figure 4. SED plume temporal evolution in latitude for a broad longitude bin −115°E to −90°E degrees (a), and in longitude at 60°N–65°N Apex latitude (b), and at 65 N–70°N Apex latitude (c) on 10 May 2024

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Figure 5. A polar view of TEC snapshots between 17:00–21:30 UT on 10 May 2024 to demonstrate the plasma density gradients TOI or the patch (see red arrows) and Polar Ionization Hole (back arrows). Corresponding GUVI O/N₂ variations along the trajectory of the TIMED are also shown at approximate times of TEC snapshots. Note that the depletion of O/N₂ inside the polar cap does not align with the region of enhanced TEC, which would suggest auroral precipitation

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Figure 6. Same as Figure 5 but for snapshots at 21:45–08:55 UT (10–11 May 2024). Yellow arrows mark the area of enhanced TEC due to auroral particle precipitation

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Figure 7. Longitudinal propagation inside the polar cap of density structures in TOI and patches (a and b), and dTEC fluctuations (c and d) over two apex latitude bins of 70°N–75°N (left) and 75°N–80°N (right) on 10 May 2024

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Figure 8. A polar view of the GUVI O/N₂ measurements at ~08:30 LT on 10−11 May 2024. Orbit-by-orbit variations is shown in the left panels; a smoothed version to fill the gaps is provided merely to show a big and rough picture of O/N₂ distribution in the polar region

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