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https://doi.org/10.5194/angeo-2024-19
© Author(s) 2024. This work is distributed under
the Creative Commons Attribution 4.0 License.
the Creative Commons Attribution 4.0 License.
https://doi.org/10.5194/angeo-2024-19
© Author(s) 2024. This work is distributed under
the Creative Commons Attribution 4.0 License.
the Creative Commons Attribution 4.0 License.
02 Dec 2024
| 02 Dec 2024
Status: this preprint is currently under review for the journal ANGEO.
The Magnetic Vortex during a Solar Eclipse
Abstract. Researchers are intensively working to understand the phenomena that remain inadequately explained in connection with solar eclipses, including wind fluctuations, gravity waves, and oscillations in the Foucault pendulum. Despite the numerous theories that have been put up to elucidate these changes, substantial evidence remains necessary to substantiate any of them. Studies indicate that these alterations transpire more frequently at the core of the shadow and are observable throughout all atmospheric strata. Nevertheless, no research has concentrated on thoroughly examining the complete lunar umbra cone, encompassing the influence of the moon’s wake phenomena. The lunar umbra cone is a common structure at both ends. This work highlights the parallels between changes in wind and gravity waves during solar eclipses and interplanetary magnetic field (IMF) lines. Building on our analysis, we propose a novel concept that offers a more cohesive and effective explanation of these phenomena during eclipses. This explanation is based on the formation of the magnetic vortex generated by the IMF lines extending from behind the moon to the Earth.
How to cite. Zoughlami, A.: The Magnetic Vortex during a Solar Eclipse, Ann. Geophys. Discuss. [preprint], https://doi.org/10.5194/angeo-2024-19, in review, 2024.
Publisher's note: Copernicus Publications remains neutral with regard to jurisdictional claims made in the text, published maps, institutional affiliations, or any other geographical representation in this preprint. The responsibility to include appropriate place names lies with the authors.
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Status: open (until 28 Feb 2025)
Comment types: AC – author | RC – referee | CC – community | EC – editor | CEC – chief editor
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RC1: 'Comment on angeo-2024-19', Anonymous Referee #1, 03 Feb 2025
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This manuscript puts forward a novel concept that the formation of the magnetic vortex generated by the interplanetary magnetic field (IMF) can explain the changes in atmospheric wind and gravity waves. The author has emphasized the similarities between atmospheric changes during solar eclipses and IMF lines. While the concept is intriguing, I am compelled to reject the paper due to concerns regarding basic physics and the lack of data support.Major comments:
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The author made a scale error when analyzing the effect of the magnetic field behind the Moon on the Earth during solar eclipses. The distance between the Earth and the Moon is 60.3 Earth radii (RE). Meanwhile, the bow shock and the dayside magnetopause are located approximately 15 RE and 10 RE from the Earth, respectively. This implies a distance of more than 45 RE from the Moon to the Earth's space environment. Considering that the radius of the Moon is only 1/4 RE, according to basic fluid and magnetohydrodynamics (MHD) theory, when the IMF interacts with the Moon as an obstacle, the size of the wake behind the Moon would be extremely limited (certainly much smaller than 45 RE). Consequently, the IMF would maintain its interplanetary state when it reaches the Earth.
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Atmospheric changes are typically directly related to the momentum and energy changes in atmospheric dynamics. The association proposed between the IMF and the atmosphere during a solar eclipse is rather arbitrary and necessitates data support from ground-based or satellite observations.
Citation: https://doi.org/10.5194/angeo-2024-19-RC1 -
AC1: 'Reply on RC1', Atef zoughlami, 09 Feb 2025
reply
I thank the referee for reviewing the manuscript and asking important questions.
Answer 1
- This study also aims to elucidate the effect of solar wind flow angles on the expansion of the magnetic field behind the Moon. Data and observations indicate that in the case of parallel flows, the magnetic field intensity increases and is conveyed over long distances along the flow direction. In contrast, in the case of perpendicular flow, the expansion of the interplanetary magnetic field (IMF) lines is confined to the region close to the Moon. For instance, one study demonstrated that the magnetic field intensity increases as the Moon aligns more with the direction of the Sun; however, the Moon’s proximity to the Sun does not necessarily guarantee that the vortex will extend over long distances, since disturbances may arise especially along lateral and edge regions that lead to its instability. In order to achieve a balance that permits the magnetic field lines to propagate over long distances, certain conditions must be met. Chief among these is that the obstructing body is oriented perpendicular to the source of the flow, resulting in a uniform distribution of the field lines in all directions (in the case of parallel solar winds). When a calm and orderly flow exists, the IMF lines follow a smooth trajectory without disturbances at the edges of the obstructing body. This results in a gentle interaction with its surface, so the lines bend smoothly over the surface with a slight inward inclination and continue to travel over long distances with an increase in their velocity relative to the initial state.This phenomenon can be compared to the flow of calm water around a rock in a river, where the water conforms to the shape of the rock harmoniously without collision or random dispersion. Given that the obstructing body (the moon) is spherical, the curved field lines preserve their original form while gradually deviating to form a conical structure that extends over long distances. This conical structure corresponds to what is known as the lunar umbra cone; indeed, both bend from nearly the same angle behind the Moon, leading the boundaries of the curved lines to approximately coincide with those of the umbra cone.In the context of fluid mechanics, this type of flow is described as “Laminar flow around a sphere." In such a state, the flow of the fluid or gas is organized and parallel along defined trajectories, free from disturbances or intersections, which allows the material to bend smoothly over long distances. Naturally, this behavior depends on the bending angle of the material behind the obstructing body and its density. Despite the extensive propagation of the field lines under laminar flow (close to natural flow conditions), disturbances and fluctuations may still occur in the lower part of the tail. During a solar eclipse when the Moon is perpendicular to the Earth, our planet plays a significant intervening role. Earth acts as a large magnet perpendicular to the vortex structure, thereby stabilizing the field lines, preventing their disintegration, and allowing them to continue along their course toward the lower part of the conical tail. This mechanism is referred to as “external field flow stabilization” or “magnetic stabilization of vortices.” Such stabilization finds applications in diverse fields, including nuclear fusion reactors, magnetic energy storage, and the optimization of electronic devices that rely on micro-magnetic materials.
In summary, any spherical body subjected to a flow generally results in the formation of vortices and disturbances in its wake; however, a particular flow angle may contribute to the formation of a stable vortex that preserves its structure. On this basis, it can be considered that a solar eclipse provides the ideal angular conditions for the Moon, leading to a specific type of flow and vortices with distinctive characteristics, with a significant contribution from Earth in achieving enhanced stability.
Answer 2
- Numerous studies conducted during solar eclipses have revealed the existence of two distinct streams around the maximum obstruction boundary within the umbra cone. Observations indicate that plasma is drawn upward at the leading edge of the shadow, whereas plasma is pushed downward at the trailing edge. This phenomenon is similarly reflected in wind behavior, with evidence of descending winds at the front of the umbra and ascending winds at its rear. Consequently, this phenomenon has been termed an “eclipse cyclone,” suggesting that the winds wrap around the center of the shadow. To dispel any doubts regarding atmospheric fluctuations and changes arising from the solar eclipse, our study incorporated pendulum experiments. These experiments confirm the presence of a novel magnetic field that accelerates the pendulum’s rotation within the umbra cone. These results are not related to momentum and energy.
- From our perspective, we propose that the IMF lines between the Sun and the Moon which traverse the Moon’s surface smoothly with a slight bending angle, might explain these as-yet-unresolved phenomena. However, we acknowledge that the manuscript requires additional experimental data, a point we have duly noted. Consequently, we have designed a new experiment, distinct from previous ones, aimed at verifying the vortex structure within the umbra cone at multiple levels (terrestrial, atmospheric, and space) to monitor rotational motion.We believe this study represents a substantial contribution to the scientific literature, especially in light of the limited existing theories on the subject. Moreover, given that solar eclipses are rare phenomena, the proposed experimental approach may enable even developing countries to pursue this research using relatively simple and cost-effective means. In conclusion, we emphasize that the proposed concept aligns with the principles of fluid mechanics and fundamental physics, and the objective of this research is to present an initial theoretical study at this stage.
Best regards.
Citation: https://doi.org/10.5194/angeo-2024-19-AC1 - This study also aims to elucidate the effect of solar wind flow angles on the expansion of the magnetic field behind the Moon. Data and observations indicate that in the case of parallel flows, the magnetic field intensity increases and is conveyed over long distances along the flow direction. In contrast, in the case of perpendicular flow, the expansion of the interplanetary magnetic field (IMF) lines is confined to the region close to the Moon. For instance, one study demonstrated that the magnetic field intensity increases as the Moon aligns more with the direction of the Sun; however, the Moon’s proximity to the Sun does not necessarily guarantee that the vortex will extend over long distances, since disturbances may arise especially along lateral and edge regions that lead to its instability. In order to achieve a balance that permits the magnetic field lines to propagate over long distances, certain conditions must be met. Chief among these is that the obstructing body is oriented perpendicular to the source of the flow, resulting in a uniform distribution of the field lines in all directions (in the case of parallel solar winds). When a calm and orderly flow exists, the IMF lines follow a smooth trajectory without disturbances at the edges of the obstructing body. This results in a gentle interaction with its surface, so the lines bend smoothly over the surface with a slight inward inclination and continue to travel over long distances with an increase in their velocity relative to the initial state.This phenomenon can be compared to the flow of calm water around a rock in a river, where the water conforms to the shape of the rock harmoniously without collision or random dispersion. Given that the obstructing body (the moon) is spherical, the curved field lines preserve their original form while gradually deviating to form a conical structure that extends over long distances. This conical structure corresponds to what is known as the lunar umbra cone; indeed, both bend from nearly the same angle behind the Moon, leading the boundaries of the curved lines to approximately coincide with those of the umbra cone.In the context of fluid mechanics, this type of flow is described as “Laminar flow around a sphere." In such a state, the flow of the fluid or gas is organized and parallel along defined trajectories, free from disturbances or intersections, which allows the material to bend smoothly over long distances. Naturally, this behavior depends on the bending angle of the material behind the obstructing body and its density. Despite the extensive propagation of the field lines under laminar flow (close to natural flow conditions), disturbances and fluctuations may still occur in the lower part of the tail. During a solar eclipse when the Moon is perpendicular to the Earth, our planet plays a significant intervening role. Earth acts as a large magnet perpendicular to the vortex structure, thereby stabilizing the field lines, preventing their disintegration, and allowing them to continue along their course toward the lower part of the conical tail. This mechanism is referred to as “external field flow stabilization” or “magnetic stabilization of vortices.” Such stabilization finds applications in diverse fields, including nuclear fusion reactors, magnetic energy storage, and the optimization of electronic devices that rely on micro-magnetic materials.
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RC2: 'Comment on angeo-2024-19', Anonymous Referee #2, 04 Feb 2025
reply
“The Magnetic Vortex during a Solar Eclipse” by Atef Zoughlami
The manuscript presented a concept for generating a magnetic vortex phenomenon during a solar eclipse. However, I cannot find any new analysis results and theoretical results and it looks like to show that the author argued just the concept. Therefore, I recommend that the author should resubmit the manuscript with significant modifications to validate the concept along with new analysis results and theoretical results.
[Major comment]
There are no new analysis results and theoretical results for validating the concept. All the results are referred from the previous works. The discussion under the present manuscript format considerably, thus seems to me to be based more on speculation than on reported facts.
Citation: https://doi.org/10.5194/angeo-2024-19-RC2 -
AC2: 'Reply on RC2', Atef zoughlami, 13 Feb 2025
reply
We thank the referee for dedicating time to reading and evaluating our paper.
- When the Moon is at its closest point to the Sun, the solar wind flow attains maximum parallelism, resulting in a uniform distribution of lines from all directions 180° behind the Moon. Because of the low density of the flowing material, a minor curve may be formed while retaining continuity and remaining extremely similar to the natural condition in terms of speed, energy, and long distances. This type of flow is known as laminar flow, and consequently, the separation angle is very near the point where the lunar shadow begins. A high-intensity magnetic field with a perpendicular orientation is required to ensure a uniform distribution of magnetic field lines, a condition provided by Earth during a solar eclipse. This also implies that the magnetic field lines align with the edges of the conical shadow structure, leading to a higher concentration of the magnetic field at the lower end of the tail. Ultimately, this curved magnetic field can affect the motion of charged particles, potentially leading to changes in wind patterns within the atmospheric layers, as observed during a solar eclipse around the lunar umbra cone.
- We agree with the referee that the submitted manuscript requires a more detailed explanation and deeper interpretation. Given that this concept is entirely novel, it currently lacks empirical results and data; however, it adheres to the laws of physics and fluid dynamics. We would be pleased to expand the discussion to address any points for improvement or to answer any questions. Additionally, we believe that certain sections can be maintained, while major revisions are warranted for the abstract, discussion and conclusions.
With sincere thanks and appreciation.
Citation: https://doi.org/10.5194/angeo-2024-19-AC2
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AC2: 'Reply on RC2', Atef zoughlami, 13 Feb 2025
reply
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Short summary
This study redefines our understanding of the factors influencing changes during solar eclipses by integrating observations of the interplanetary magnetic field (IMF) lines, winds, and gravity waves within the lunar umbra cone. This integration leads to a novel theory that reveals a magnetic vortex in the moon's wake that explains the origins of these changes and their impact on the atmosphere, winds, and Foucault's pendulum.
This study redefines our understanding of the factors influencing changes during solar eclipses...