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There’s no evidence that Earth’s climate has been significantly impacted by the last three magnetic field excursions, nor by any excursion event within at least the last 2.8 million years.

Physical Principles

1. Insufficient Energy in Earth’s Upper Atmosphere

Electromagnetic currents exist within Earth’s upper atmosphere. But the energy driving the climate system in the upper atmosphere is, on global average, a minute fraction of the energy that drives the climate system at Earth’s surface. Its magnitude is typically less than one to a few milliwatts per square meter. To put that into context, the energy budget at Earth’s surface is about 250 to 300 watts per square meter. In the long run, the energy that governs Earth’s upper atmosphere is about 100,000 times less than the amount of energy driving the climate system at Earth’s surface. There is simply not enough energy aloft to have an influence on climate down where we live.

2. Air Isn’t Ferrous

Finally, changes and shifts in Earth’s magnetic field polarity don’t impact weather and climate for a fundamental reason: air isn’t ferrous.

Ferrous? Say what?? Bueller? Bueller?

Ferrous means “containing or consisting of iron.” While iron in volcanic ash is transported in the atmosphere, and small quantities of iron and iron compounds generated by human activities are a source of air pollution in some urban areas, iron isn’t a significant component of Earth’s atmosphere. There’s no known physical mechanism capable of connecting weather conditions at Earth’s surface with electromagnetic currents in space.

Thermal and compositional structure of the atmosphere.
Thermal and compositional structure of the atmosphere. The upper atmosphere, comprising the mesosphere, thermosphere, and embedded ionosphere, absorbs all incident solar radiation at wavelengths less than 200 nanometers (nm). Most of that absorbed radiation is ultimately returned to space via infrared emissionsfrom carbon dioxide (CO2) and nitric oxide (NO) molecules. The stratospheric ozone layer absorbs radiation between 200 and 300 nm.

The plot on the left shows the typical global-average thermal structure of the atmosphere when the flux of solar radiation is at the minimum and maximum values of its 11-year cycle. The plot on the right shows the density of nitrogen (N2), oxygen (O2), and atomic oxygen (O), the three major neutral species in the upper atmosphere, along with the free electron (e-) density, which is equal to the combined density of the various ion species. The F, E, and D regions of the ionosphere are also indicated, as is the troposphere, the atmosphere’s lowest region. Credit: Naval Research Laboratory/J. Emmert

Solar storms and their electromagnetic interactions only impact Earth’s ionosphere, which extends from the lowest edge of the mesosphere (about 31 miles or 50 kilometers above Earth’s surface) to space, around 600 miles (965 kilometers) above the surface. They have no impact on Earth’s troposphere or lower stratosphere, where Earth’s surface weather, and subsequently its climate, originate.

In short, when it comes to climate, variations in Earth’s magnetic field are nothing to get charged up about.