Schumann Resonances are radio waves, caused primarily by lightning discharge between the Ionosphere (upper atmosphere), and the Earth Ground.
Lightning discharge is a release of high voltage from the upper atmosphere, to Earth ground. This initial discharge, a release of high voltage into the immediate atmosphere creates a spike in atmospheric electromagnetics.
This voltage spike is seen as Amplitude on the charts and spectrogram. Amplitude in Intensity, or "electrical loudness"; as measured in deci-Bels. These electrical discharges then propagate-out into the immediate environment.
After this release of voltage, the electric charge radiates, or propagates out into the lower atmosphere, eventually dissipating into Schumann Resonances. These resonances are standing waves. Standing waves are created by multiple fundamental waves, which collide into each other. Resonances are standing waves, which "hum" or oscillate in place.
Schumann resonances do not wander; these do not propagate. Schumann resonances are standing waves, which vibrate, or oscillate in place. Even though this phenomena happens all around the world, the relative strength is varied.
The process of understanding Schumann resonances is complex. The easier, softer way has been given to the people, through the invention of the "ascension-based" narrative. The powers-that-be have given the masses the easier way of grasping this principle.
Seemingly, with all things these days, there's an over-abundance of rhetoric, which is physically disconnected from the actual thing it's referencing.
It's a common issue for people new into this study, to actually ignore what the SR is, in place of the contrived, easier, softer way of the "new age" version. It's a bit of a red herring to study the sun, in reference to the SR; without first understanding the role of the ionosphere.
The topic of the Ionosphere is complex. There's ALOT to this. I waned to do a quick introduction to this important element of the overall process.
Thank you for being here. Thank you for your patience.
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Ionosphere.
The ionosphere is the ionized part of the upper atmosphere of Earth, from about 48 km (30 mi) to 965 km (600 mi) above sea level, a region that includes the thermosphere and parts of the mesosphere and exosphere.
The ionosphere is ionized by solar radiation.
It plays an important role in atmospheric electricity and forms the inner edge of the magnetosphere.
It has practical importance because, among other functions, it influences radio propagation to distant places on Earth.
Geophysics
The ionosphere is a shell of electrons and electrically charged atoms and molecules that surrounds the Earth, stretching from a height of about 50 km (30 mi) to more than 1,000 km (600 mi).
It exists primarily due to ultraviolet radiation from the Sun.
The lowest part of the Earth's atmosphere, the troposphere extends from the surface to about 10 km (6 mi).
Above that is the stratosphere, followed by the mesosphere. In the stratosphere incoming solar radiation creates the ozone layer.
At heights of above 80 km (50 mi), in the thermosphere, the atmosphere is so thin that free electrons can exist for short periods of time before they are captured by a nearby positive ion.
The number of these free electrons is sufficient to affect radio propagation.
This portion of the atmosphere is partially ionized and contains a plasma which is referred to as the ionosphere.
Ultraviolet (UV), X-ray and shorter wavelengths of solar radiation are ionizing, since photons at these frequencies contain sufficient energy to dislodge an electron from a neutral gas atom or molecule upon absorption.
In this process the light electron obtains a high velocity so that the temperature of the created electronic gas is much higher (of the order of thousand K) than the one of ions and neutrals.
The reverse process to ionization is recombination, in which a free electron is "captured" by a positive ion. Recombination occurs spontaneously. It causes the emission of a photon carrying away the energy produced upon recombination.
As gas density increases at lower altitudes, the recombination process prevails, since the gas molecules and ions are closer together.
The balance between these two processes determines the quantity of ionization present.
Ionization depends primarily on the Sun and its Extreme Ultraviolet (EUV) and X-ray irradiance which varies strongly with solar activity. The more magnetically active the Sun is, the more sunspot active regions there are on the Sun at any one time.
Sunspot active regions are the source of increased coronal heating and accompanying increases in EUV and X-ray irradiance, particularly during episodic magnetic eruptions that include solar flares that increase ionization on the sunlit side of the Earth and solar energetic particle events that can increase ionization in the polar regions.
Thus the degree of ionization in the ionosphere follows both a diurnal (time of day) cycle and the 11-year solar cycle.
There is also a seasonal dependence in ionization degree since the local winter hemisphere is tipped away from the Sun, thus there is less received solar radiation.
Radiation received also varies with geographical location (polar, auroral zones, mid-latitudes, and equatorial regions).
There are also mechanisms that disturb the ionosphere and decrease the ionization.
Layers of ionization
At night the F layer is the only layer of significant ionization present, while the ionization in the E and D layers is extremely low.
During the day, the D and E layers become much more heavily ionized, as does the F layer, which develops an additional, weaker region of ionisation known as the F1 layer.
The F2 layer persists by day and night and is the main region responsible for the refraction and reflection of radio waves.
D layer
The D layer is the innermost layer, 48 km (30 mi) to 90 km (56 mi) above the surface of the Earth. Ionization here is due to Lyman series-alpha hydrogen radiation at a wavelength of 121.6 nanometre (nm) ionizing nitric oxide (NO).
In addition, solar flares can generate hard X-rays (wavelength < 1 nm) that ionize N2 and O2.
Recombination rates are high in the D layer, so there are many more neutral air molecules than ions.
Medium frequency (MF) and lower high frequency (HF) radio waves are significantly attenuated within the D layer, as the passing radio waves cause electrons to move, which then collide with the neutral molecules, giving up their energy.
Lower frequencies experience greater absorption because they move the electrons farther, leading to greater chance of collisions. This is the main reason for absorption of HF radio waves, particularly at 10 MHz and below, with progressively less absorption at higher frequencies.
This effect peaks around noon and is reduced at night due to a decrease in the D layer's thickness; only a small part remains due to cosmic rays.
A common example of the D layer in action is the disappearance of distant AM broadcast band stations in the daytime.
During solar proton events, ionization can reach unusually high levels in the D-region over high and polar latitudes.
Such very rare events are known as Polar Cap Absorption (or PCA) events, because the increased ionization significantly enhances the absorption of radio signals passing through the region.[18]
In fact, absorption levels can increase by many tens of dB during intense events, which is enough to absorb most (if not all) transpolar HF radio signal transmissions.
Such events typically last less than 24 to 48 hours.
E layer: Kennelly–Heaviside layer
The E layer is the middle layer, 90 km (56 mi) to 150 km (93 mi) above the surface of the Earth. Ionization is due to soft X-ray (1–10 nm) and far ultraviolet (UV) solar radiation ionization of molecular oxygen (O2).
Normally, at oblique incidence, this layer can only reflect radio waves having frequencies lower than about 10 MHz and may contribute a bit to absorption on frequencies above.
However, during intense sporadic E events, the Es layer can reflect frequencies up to 50 MHz and higher.
The vertical structure of the E layer is primarily determined by the competing effects of ionization and recombination.
At night the E layer weakens because the primary source of ionization is no longer present.
After sunset an increase in the height of the E layer maximum increases the range to which radio waves can travel by reflection from the layer.
This region is also known as the Kennelly–Heaviside layer or simply the Heaviside layer. Its existence was predicted in 1902 independently and almost simultaneously by the American electrical engineer Arthur Edwin Kennelly (1861–1939) and the British physicist Oliver Heaviside (1850–1925). In 1924 its existence was detected by Edward V. Appleton and Miles Barnett.
E-s layer
The E-s layer (sporadic E-layer) is characterized by small, thin clouds of intense ionization, which can support reflection of radio waves, frequently up to 50 MHz and rarely up to 450 MHz.
Sporadic-E events may last for just a few minutes to many hours. Sporadic E propagation makes VHF-operating by radio amateurs very exciting when long distance propagation paths that are generally unreachable "open up" to two-way communication.
There are multiple causes of sporadic-E that are still being pursued by researchers.
This propagation occurs every day during June and July in northern hemisphere mid-latitudes when high signal levels are often reached. The skip distances are generally around 1,640 km (1,020 mi).
F layer
The F layer or region, also known as the Appleton–Barnett layer, extends from about 150 km (93 mi) to more than 500 km (310 mi) above the surface of Earth.
It is the layer with the highest electron density, which implies signals penetrating this layer will escape into space.
Electron production is dominated by extreme ultraviolet (UV, 10–100 nm) radiation ionizing atomic oxygen.
The F layer consists of one layer (F2) at night, but during the day, a secondary peak (labelled F1) often forms in the electron density profile.
Because the F2 layer remains by day and night, it is responsible for most skywave propagation of radio waves and long distance high frequency (HF, or shortwave) radio communications.
Above the F layer, the number of oxygen ions decreases and lighter ions such as hydrogen and helium become dominant.
This region above the F layer peak and below the plasmasphere is called the topside ionosphere.
source: ( https://en.wikipedia.org/wiki/Ionosphere )
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