Space weather impacts radio communication in a number of ways. At frequencies in the 1 to 30 MHz range (HF radio), the changes in ionospheric density and structure modify the transmission path and even block transmission of HF radio signals completely.

In the red image (304 Angstroms), we can see very small spicules—jets of solar material—and some small prominences at the sun’s edge, which are not easy to see in the other two images. In the second sequence (193 Angstroms), we can readily observe the large and dark coronal hole, though it is difficult to make out in the others. In the third image (171 Angstroms), we can see strands of plasma waving above the surface.

Space Weather describes the variations in the space environment between the sun and Earth.

In particular, Space Weather describes the phenomena that impact systems and technologies in orbit and on Earth.

There are several types of space weather that can impact HF radio communication. In a typical sequence of space weather storms, the first impacts are felt during the solar flare itself. The solar x-rays from the sun penetrate to the bottom of the ionosphere (to around 80 km). There the x-ray photons ionize the atmosphere and create an enhancement of the D layer of the ionosphere.

This enhanced D-layer acts both as a reflector of radio waves at some frequencies and an absorber of waves at other frequencies. The Radio Blackout associated with solar flares occurs on the dayside region of Earth and is most intense when the sun is directly overhead.

CURRENT D REGION ABSORPTION PREDICTION

CURRENT SPACE WATHER OBSERVATIONS

SOLAR X-RAY FLUX

The GOES X-ray plots shown here are used to track solar activity and solar flares. Large solar X-ray flares can change the Earth’s ionosphere, which blocks high-frequency (HF) radio transmissions on the sunlit side of the Earth. Solar flares are also associated with Coronal Mass Ejections (CMEs) which can ultimately lead to geomagnetic storms.

While increasing SFI may be good for HF propagation, it also tends to correspond with high Ap and K indices, which cause D-Layer absorption and noisy band condition.

SOLAR PROTON FLUX

Protons are charged particles and are therefore influenced by magnetic fields

GEO MAGNETIC ACTIVITY

In a simplified view, geomagnetic activities are the product of the interaction between the solar wind and magnetosphere. The Kp Index (p = planetary) is the measure.

The K-index, and by extension the Planetary K-index, are used to characterize the magnitude of geomagnetic storms. Kp is an excellent indicator of disturbances in the Earth’s magnetic field and is used by SWPC to decide whether geomagnetic alerts and warnings need to be issued for users who are affected by these disturbances.

The principal users affected by geomagnetic storms are the electrical power grid, spacecraft operations, users of radio signals that reflect off of or pass through the ionosphere, and observers of the aurora.

24 HOUR SOLAR ACTIVITY SUMMARY

LATEST VIDEO

This channel highlights the outer atmosphere of the Sun – called the corona – as well as hot flare plasma. Hot active regions, solar flares, and coronal mass ejections will appear bright here. The dark areas – called coronal holes – are places where very little radiation is emitted, yet are the main source of solar wind particles.

Space weather can occur anywhere from the surface of the sun to the surface of Earth. 

As a space weather storm leaves the sun, it passes through the corona and into the solar wind. When it reaches Earth, it energizes Earth’s magnetosphere and accelerates electrons and protons down to Earth’s magnetic field lines where they collide with the atmosphere and ionosphere, particularly at high latitudes.

 Each component of space weather impacts a different technology.

Source: NOAA

The Sun releases a constant stream of particles and magnetic fields called the solar wind. This solar wind slams worlds across the solar system with particles and radiation – which can stream all the way to planetary surfaces unless thwarted by an atmosphere, magnetic field, or both. Here’s how these solar particles interact with a few select planets and other celestial bodies. The solar wind is mostly deflected by our magnetic field, but sometimes, when intense, some of it can leak through. Once in near-Earth space, the particles can trigger aurora near the poles.

The top two panels show the latest global Total Electron Content (TEC) and Maximum Usable Frequency (MUF) as forecasted by the WAM-IPE. The bottom two panels show the anomaly in TEC and MUF taking the difference between the latest values and a 10-day running average at the same universal time. The forecast is updated with the latest real-time and forecast solar and geomagnetic drivers at 0, 6, 12 & 18 UT.

Click the image below to see a 3 day animation of the prediction.