Despite the importance for understanding the nature of the geomagnetic field, and especially its potential for radically disrupting modern civilization [1], virtually all scientific publications relating to it are based upon the false assumption that the geomagnetic field is generated in the Earth’s fluid core. By adhering to an outmoded paradigm, members of the geoscience community have potentially exposed humanity to globally devastating risks, leaving it unprepared for an inevitable geomagnetic field collapse. There is no scientific reason to believe that the geomagnetic field is generated within the fluid core. Convection is physically impossible in the fluid core due to its compression by the weight above and its inability to sustain an adverse temperature gradient. There is no evidence of ongoing inner core growth to provide energy to drive thermal convection or to cause compositional convection. Moreover, there is no mechanism to account for magnetic reversals and no means for magnetic seed-field production within the fluid core to initiate dynamo amplification. Earth’s nuclear georeactor, seat of the geomagnetic field, has none of the problems inherent in putative fluid-core geomagnetic field production. With a mass of about one ten-millionth that of the fluid core, georeactor sub-shell convection can potentially be disrupted by great planetary trauma, such as an asteroid impact, or by major solar outbursts or even by human activities, for example, by deliberate electromagnetic disturbance of the near-Earth environment, including the Van Allen belts. Furthermore, sub-shell convection disruption might trigger surface geophysical disasters, such as supervolcano eruptions [2-4]. Scientists have a fundamental responsibility to tell the truth and to provide scientific understanding that benefits humanity. Reasons Why Geomagnetic Field Generation is Physically Impossible in Earth’s Fluid Core | Advances in Social Sciences Research Journal Reasons Why Geomagnetic Field Generation is Physically Impossible in Earth’s Fluid Core Authors J. Marvin Herndon Transdyne Corporation DOI: https://doi.org/10.14738/assrj.85.10184 Keywords: Corona ejections; Magnetic reversals; Geomagnetic storms; Geomagnetic collapse; Solar wind; Super volcano; Communications disruption; Inner core; Convection. Abstract Despite the importance for understanding the nature of the geomagnetic field, and especially its potential for radically disrupting modern civilization [1], virtually all scientific publications relating to it are based upon the false assumption that the geomagnetic field is generated in the Earth’s fluid core. By adhering to an outmoded paradigm, members of the geoscience community have potentially exposed humanity to globally devastating risks, leaving it unprepared for an inevitable geomagnetic field collapse. There is no scientific reason to believe that the geomagnetic field is generated within the fluid core. Convection is physically impossible in the fluid core due to its compression by the weight above and its inability to sustain an adverse temperature gradient. There is no evidence of ongoing inner core growth to provide energy to drive thermal convection or to cause compositional convection. Moreover, there is no mechanism to account for magnetic reversals and no means for magnetic seed-field production within the fluid core to initiate dynamo amplification. Earth’s nuclear georeactor, seat of the geomagnetic field, has none of the problems inherent in putative fluid-core geomagnetic field production. With a mass of about one ten-millionth that of the fluid core, georeactor sub-shell convection can potentially be disrupted by great planetary trauma, such as an asteroid impact, or by major solar outbursts or even by human activities, for example, by deliberate electromagnetic disturbance of the near-Earth environment, including the Van Allen belts. Furthermore, sub-shell convection disruption might trigger surface geophysical disasters, such as super-volcano eruptions [2-4]. Scientists have a fundamental responsibility to Reasons Why Geomagnetic Field Generation is Physically Impossible in Earth’s Fluid Core. Advances in Social Sciences Research Journal , 8 (5), 84–97. https://doi.org/10.14738/assrj.85.10184 More Citation Formats ACM ACS APA ABNT Chicago Harvard IEEE MLA Turabian Vancouver Download Citation Endnote/Zotero/Mendeley (RIS) BibTeX Issue Vol. 8 No. 5 (2021): Advances in Social Sciences Research Journal Section Articles Most read articles by the same author(s) J. 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Solar particle events (SPEs) are short-lived bursts of high-energy particles from the solar atmosphere and are widely recognized as posing significant economic risks to modern society. Most SPEs are relatively weak and have minor impacts on the Earth's environment, but historic records contain much stronger SPEs which have the potential to alter atmospheric chemistry, impacting climate and biological life. The impacts of such strong SPEs would be far more severe when the Earth's protective geomagnetic field is weak, such as during past geomagnetic excursions or reversals. Here, we model the impacts of an extreme SPE under different geomagnetic field strengths, focusing on changes in atmospheric chemistry and surface radiation using the atmosphere-ocean-chemistry-climate model SOCOL3-MPIOM and the radiation transfer model LibRadtran. Under current geomagnetic conditions, an extreme SPE would increase NO_x concentrations in the polar stratosphere and mesosphere, causing reductions in extratropical stratospheric ozone lasting for about a year. In contrast, with no geomagnetic field, there would be a substantial increase in NO_x throughout the entire atmosphere, resulting in severe stratospheric ozone depletion for several years. The resulting ground-level ultraviolet (UV) radiation would remain elevated for up to 6 y, leading to increases in UV index up to 20 to 25% and solar-induced DNA damage rates by 40 to 50%. The potential evolutionary impacts of past extreme SPEs remain an important question, while the risks they pose to human health in modern conditions continue to be underestimated. Potential consequences include serious health hazards and longer-term climatic and evolutionary impacts. Solar particle events (SPEs) are short-lived bursts of high-energy particles from the solar atmosphere and are widely recognized as posing significant economic risks to modern society. Most SPEs are relatively weak and have minor impacts on the Earth’s environment, but historic records contain much stronger SPEs which have the potential to alter atmospheric chemistry, impacting climate and biological life. The impacts of such strong SPEs would be far more severe when the Earth’s protective geomagnetic field is weak, such as during past geomagnetic excursions or reversals. The resulting ground-level ultraviolet (UV) radiation would remain elevated for up to 6 y, leading to increases in UV index up to 20 to 25% and solar-induced DNA damage rates by 40 to 50%. The potential evolutionary impacts of past extreme SPEs remain an important question, while the risks they pose to human health in modern conditions continue to be underestimated. These periods include events such as geomagnetic polarity reversals (when the magnetic poles switch) and geomagnetic field excursions (a pronounced reduction of geomagnetic field strength, but without long-term polarity inversion), and can be observed back as far as the Ediacaran period ( 22 , 23 ). During such phases of greatly reduced geomagnetic field strength, the biophysical consequences of SPEs could be very large, as solar particles would precipitate over a much larger proportion of the Earth’s surface, including lower latitudes. The clear-sky erythemal irradiance is quantified with the UV Index or UVI, which is a measure of the intensity of UV radiation in terms of causing sunburn in human skin. Our models predict that a SPE under modern conditions would result in a significant increase in erythemal radiation across all continents ( Fig. 6 ). The relative increase is ~5% over North America, Europe, and Asia, and 2 to 3% over South America, Africa, and Australia, persisting for 2 to 3 y after the SPE. However, during a geomagnetic excursion there are much more severe global increases in the UV Index, with a 25% increase in the first year over Europe, North America, and Asia. As a result, using the UVI to quantify ocular damage has been shown to considerably underestimate the risk of ocular damage from UV-B exposure [particularly in the ~290 nm wavelength range most impacted by atmospheric ozone decrease; ( 58 )]. This risk can be increased further by reflective surfaces such as snow cover, which can reflect up to 88% of solar UV-B radiation ( 59 ). Clearly, photokeratitis could pose a significant risk to human populations when a SPE occurs during weak geomagnetic field conditions. Vitamin D Production. While short-lived, these impacts are likely to cause complex interactions with potentially longer global effects. Within animals, such high UV levels would be associated with elevated rates of sunburn, cataracts, and DNA damage. These impacts are likely to be particularly severe for humans who lack skin coverings or thick hides, leading to increased risks of skin cancer, cataracts, and impaired immune function as long-term impacts ( 52 ). The most immediate negative impact for many animal groups would potentially be damage to the eyes, which would be heightened in environments with reflective surfaces such as snow, savannah, water, or sand ( 58 , 87 ). In the case of humans, the high UVI (25% increase) exposure could quickly lead to snow blindness, which can manifest anywhere from 30 min to 12 h after the actual exposure ( 87 ). The resulting intense pain from exposure to light, severe headaches, and blurry or complete loss of vision would be debilitating to As Earth’s climate continues to change, ecosystems and human societies will become more vulnerable to the impacts of changes in geomagnetic field strength. Future changes in atmospheric circulation and temperature ( 70 ) will impact the dynamics of the ozone layer, which could worsen the impact of increased UV radiation. Understanding the impact of extreme SPEs on our atmosphere and developing strategies to address these risks will be important for safeguarding our technological infrastructure and the welfare of the global population. Materials and Methods SOCOL3-MPIOM Model Setup.

In the recent geological past, Earth's magnetic field reduced to ~10% of the modern values and the magnetic poles shifted away from the geographic poles, causing the Laschamps geomagnetic excursion, about 41 millennia ago. The excursion lasted ~2000 years, with dipole strength reduction and tilting spanning 300 years. During this period, the geomagnetic field's multipolarity resembled outer planets, causing rapid magnetospheric changes. To our knowledge, this study presents the first space plasma analysis of the excursion, linking the geomagnetic field, magnetospheric system, and upper atmosphere in sequence using feedback channels for distinct temporal epochs. A three-dimensional reconstruction of Earth's geospace system shows that these shifts affected auroral regions and open magnetic field lines, causing them to expand and wander toward lower latitudes. These changes likely altered the upper atmosphere's composition and influenced anthropological progress during that era. Looking through a modern lens, such an event would disrupt contemporary technology, including communications and satellite infrastructure. Distributed under a Creative Commons Attribution License 4.0 (CC BY). This is an open-access article distributed under the terms of the Creative Commons Attribution license , which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Abstract In the recent geological past, Earth’s magnetic field reduced to ~10% of the modern values and the magnetic poles shifted away from the geographic poles, causing the Laschamps geomagnetic excursion, about 41 millennia ago. The excursion lasted ~2000 years, with dipole strength reduction and tilting spanning 300 years. On certain occasions, the geomagnetic field changes rapidly over the time span of a few millennia; these events are called geomagnetic excursions ( 25 ) (henceforth referred to as excursions). Excursions are similar to geomagnetic reversals but occur over shorter timescales ( 24 ). They cause the intrinsic field strength to diminish and the magnetic tilt to change ( 25 ), rapidly relocating the magnetic poles over vast distances, even within a human lifetime ( 26 ). By contrast, the duration of the most recent reversal, Matuyama-Brunhes reversal, is estimated to be in the order of 20 to 30 thousand years ( 27 ). Thus, it is virtually certain that the notable fluctuations observed in the geomagnetic field during the Laschamps excursion would have triggered a marked transformation in Earth’s magnetospheric configuration. Recent investigations into Earth’s magnetospheric structure during the Matuyama-Brunhes reversal—the most recent geomagnetic reversal that took place 778 ka—uncovered a substantial reduction in the magnetosphere’s size and the emergence of numerous regions where the magnetic field lines interact and release energy over a period spanning multiple millenia ( 34 ). By 40.531 ka, despite a muted dipole strength (∼19% of modern values), the magnetosphere started to show signs of recovery (see Fig. 2E ), with These charged particles, upon collision with neutral atoms within Earth’s atmosphere ( 9 ), ignite the ethereal display known as the aurorae or the Northern/Southern Lights. Primarily concentrated around the geomagnetic poles, the aurora finds its most pronounced manifestation near the delineating boundary between zones characterized by open and closed field lines ( 45 ). In doing so, it forms a ring-shaped contour surrounding the geomagnetic poles, commonly referred to as the auroral oval. Variations in magnetospheric shape and structure instigate the auroral oval in both the Northern Hemisphere and Southern Hemisphere to fluctuate. This resulted in the expansion of the polar region encompassed by open field lines and resulted in the subsequent expansion of the aurora ( 26 ). 2) Rapid variations in the dipole tilt angle over a few centuries enabled the geomagnetic poles to be severely inclined, causing the location of the open-closed field line boundary and, by extension, the auroral oval to wander across the globe. Figure 3 illustrates the transformative shifts across the Northern Hemisphere and Southern Hemisphere auroral zones during the excursion. 1 , whereas subplots ( F to J ) showcase auroral coverage in the Southern Hemisphere during the same epochs. (Top projection in each subplot) Auroral energy flux contours are represented at 1.5 R E (10,000 km), with values saturated at 10 mW/m 2 . (Bottom projection in each subplot) The auroral oval (light green) and aggregate open field line zones (dark green) are projected at atmospheric altitudes (110 km) for each epoch, displayed over an orthographic globe projection. Red lines indicate the trajectory of the geomagnetic poles, based on the axial dipole tilt. Considering the probable impact of the Laschamps excursion on early humans and their way of life, a similar event today would likely have dire consequences for modern humans. Despite the gradual nature of the geomagnetic variations, they were more extreme than those caused by the strongest space weather events on record ( 78 ). The ramifications of a Laschamps-like magnetospheric configuration and auroral oval would reverberate across all facets of modern communication, satellite infrastructure, and intercontinental travel. The underlying principles of the numerical models and their usage in this investigation are described in the following. Paleomagnetic field models Reconstructions on the Earth’s magnetic field variations on long multimillennial timescales are important to understand the source of the geomagnetic field and its effects on the environment and climate. Data that provide information on the paleomagnetic field come from geological archives, volcanic rocks, and sediments. Continuous progress in compiling new data enables us to model the field on even longer timescales, from human civilization to millions of years ( 82 ).