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The Day‐Side Magnetic Reconnection Rate and Cusp Ion Dispersion During the May 2024 Geomagnetic Storm.

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Title: The Day‐Side Magnetic Reconnection Rate and Cusp Ion Dispersion During the May 2024 Geomagnetic Storm.
Authors: Burkholder, B. L.1,2 (AUTHOR) blburkholder@alaska.edu, Zou, Y.3 (AUTHOR), Chen, L.‐J.2 (AUTHOR), da Silva, D. E.1,2 (AUTHOR), Nykyri, K.4 (AUTHOR), Ma, X.4 (AUTHOR), DesJardin, I.2,5 (AUTHOR), Huang, Y.‐M.2,6 (AUTHOR), Dorelli, J.2 (AUTHOR), Bessho, N.2,6 (AUTHOR), Merkin, S.3 (AUTHOR), Chartier, A.3 (AUTHOR), Sorathia, K.3 (AUTHOR), Pham, K.7 (AUTHOR), Shepherd, S. G.8 (AUTHOR)
Source: Journal of Geophysical Research. Space Physics. Apr2026, Vol. 131 Issue 4, p1-19. 19p.
Subject Terms: *Magnetic storms, Magnetic reconnection, Interplanetary magnetic fields, Magnetosphere, Solar wind, Coronal mass ejections, Space environment
Abstract: During intense space weather events, magnetic flux can be rapidly eroded from the Earth's day‐side magnetosphere, potentially exposing satellites as low as geosynchronous orbit (∼5.6 RE ${\mathrm{R}}_{E}$ altitude) directly to magnetosheath plasma. This was observed during the 10–11 May 2024 geomagnetic storm, the most severe storm to have occurred in over two decades. High interplanetary magnetic field (IMF) strength and solar wind dynamic pressure within multiple interacting coronal mass ejections resulted in strongly driven magnetic reconnection at the day‐side magnetopause. A Multiscale Atmosphere Geospace Environment (MAGE) simulation of the May 2024 geomagnetic storm shows the day‐side magnetopause reconnection rate reached >5 ${ >} 5$ mV/m during two different intervals of storm‐time southward IMF, a factor of at least 5 larger than quiet time. One of the selected intervals also has a significant By ${\mathrm{B}}_{y}$ component of the IMF, which leads to a large component x‐line on the day‐side magnetopause. Super Dual Auroral Radar Network radar observations during the nonzero By ${\mathrm{B}}_{y}$ interval infer reconnection rates up to 5 mV/m, consistent with the simulation. Simulated cusp ion test particle dispersions estimate reconnection rates of ∼3.5 ${\sim} 3.5$ mV/m during the zero By ${\mathrm{B}}_{y}$ interval and ∼2.5 ${\sim} 2.5$ mV/m during the nonzero By ${\mathrm{B}}_{y}$ interval. Key Points: Global simulations and observations show the noon open‐closed boundary reached <63° ${< } 63{}^{\circ}$ magnetic latitude during the May 2024 geomagnetic stormSimulated storm‐time reconnection rates are >5 ${ >} 5$ mV/m with strong southward interplanetary magnetic field (IMF), compared to ∼1 mV/m quiet timeSimulated cusp ion dispersions approximate storm‐time reconnection rates 3−5 mV/m during strong southward IMF, and 2−3 mV/m with By∼|Bz| ${\mathrm{B}}_{y}\sim \vert {B}_{z}\vert $ [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: The Day‐Side Magnetic Reconnection Rate and Cusp Ion Dispersion During the May 2024 Geomagnetic Storm.
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  Data: &lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Burkholder%2C+B%2E+L%2E%22&quot;&gt;Burkholder, B. L.&lt;/searchLink&gt;&lt;relatesTo&gt;1,2&lt;/relatesTo&gt; (AUTHOR)&lt;i&gt; blburkholder@alaska.edu&lt;/i&gt;&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Zou%2C+Y%2E%22&quot;&gt;Zou, Y.&lt;/searchLink&gt;&lt;relatesTo&gt;3&lt;/relatesTo&gt; (AUTHOR)&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Chen%2C+L%2E‐J%2E%22&quot;&gt;Chen, L.‐J.&lt;/searchLink&gt;&lt;relatesTo&gt;2&lt;/relatesTo&gt; (AUTHOR)&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22da+Silva%2C+D%2E+E%2E%22&quot;&gt;da Silva, D. E.&lt;/searchLink&gt;&lt;relatesTo&gt;1,2&lt;/relatesTo&gt; (AUTHOR)&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Nykyri%2C+K%2E%22&quot;&gt;Nykyri, K.&lt;/searchLink&gt;&lt;relatesTo&gt;4&lt;/relatesTo&gt; (AUTHOR)&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Ma%2C+X%2E%22&quot;&gt;Ma, X.&lt;/searchLink&gt;&lt;relatesTo&gt;4&lt;/relatesTo&gt; (AUTHOR)&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22DesJardin%2C+I%2E%22&quot;&gt;DesJardin, I.&lt;/searchLink&gt;&lt;relatesTo&gt;2,5&lt;/relatesTo&gt; (AUTHOR)&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Huang%2C+Y%2E‐M%2E%22&quot;&gt;Huang, Y.‐M.&lt;/searchLink&gt;&lt;relatesTo&gt;2,6&lt;/relatesTo&gt; (AUTHOR)&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Dorelli%2C+J%2E%22&quot;&gt;Dorelli, J.&lt;/searchLink&gt;&lt;relatesTo&gt;2&lt;/relatesTo&gt; (AUTHOR)&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Bessho%2C+N%2E%22&quot;&gt;Bessho, N.&lt;/searchLink&gt;&lt;relatesTo&gt;2,6&lt;/relatesTo&gt; (AUTHOR)&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Merkin%2C+S%2E%22&quot;&gt;Merkin, S.&lt;/searchLink&gt;&lt;relatesTo&gt;3&lt;/relatesTo&gt; (AUTHOR)&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Chartier%2C+A%2E%22&quot;&gt;Chartier, A.&lt;/searchLink&gt;&lt;relatesTo&gt;3&lt;/relatesTo&gt; (AUTHOR)&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Sorathia%2C+K%2E%22&quot;&gt;Sorathia, K.&lt;/searchLink&gt;&lt;relatesTo&gt;3&lt;/relatesTo&gt; (AUTHOR)&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Pham%2C+K%2E%22&quot;&gt;Pham, K.&lt;/searchLink&gt;&lt;relatesTo&gt;7&lt;/relatesTo&gt; (AUTHOR)&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Shepherd%2C+S%2E+G%2E%22&quot;&gt;Shepherd, S. G.&lt;/searchLink&gt;&lt;relatesTo&gt;8&lt;/relatesTo&gt; (AUTHOR)
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  Label: Abstract
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  Data: During intense space weather events, magnetic flux can be rapidly eroded from the Earth&#39;s day‐side magnetosphere, potentially exposing satellites as low as geosynchronous orbit (∼5.6 RE ${\mathrm{R}}_{E}$ altitude) directly to magnetosheath plasma. This was observed during the 10–11 May 2024 geomagnetic storm, the most severe storm to have occurred in over two decades. High interplanetary magnetic field (IMF) strength and solar wind dynamic pressure within multiple interacting coronal mass ejections resulted in strongly driven magnetic reconnection at the day‐side magnetopause. A Multiscale Atmosphere Geospace Environment (MAGE) simulation of the May 2024 geomagnetic storm shows the day‐side magnetopause reconnection rate reached &gt;5 ${ &gt;} 5$ mV/m during two different intervals of storm‐time southward IMF, a factor of at least 5 larger than quiet time. One of the selected intervals also has a significant By ${\mathrm{B}}_{y}$ component of the IMF, which leads to a large component x‐line on the day‐side magnetopause. Super Dual Auroral Radar Network radar observations during the nonzero By ${\mathrm{B}}_{y}$ interval infer reconnection rates up to 5 mV/m, consistent with the simulation. Simulated cusp ion test particle dispersions estimate reconnection rates of ∼3.5 ${\sim} 3.5$ mV/m during the zero By ${\mathrm{B}}_{y}$ interval and ∼2.5 ${\sim} 2.5$ mV/m during the nonzero By ${\mathrm{B}}_{y}$ interval. Key Points: Global simulations and observations show the noon open‐closed boundary reached &lt;63&#176; ${&lt; } 63{}^{\circ}$ magnetic latitude during the May 2024 geomagnetic stormSimulated storm‐time reconnection rates are &gt;5 ${ &gt;} 5$ mV/m with strong southward interplanetary magnetic field (IMF), compared to ∼1 mV/m quiet timeSimulated cusp ion dispersions approximate storm‐time reconnection rates 3−5 mV/m during strong southward IMF, and 2−3 mV/m with By∼|Bz| ${\mathrm{B}}_{y}\sim \vert {B}_{z}\vert $ [ABSTRACT FROM AUTHOR]
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  Data: &lt;i&gt;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&#39;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.&lt;/i&gt; (Copyright applies to all Abstracts.)
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