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Effective SSNe from fo,F2 Measurements,
Solar Active Regions Earth- and Far-Side
Strength & ETA of Far-Side Active Regions
Sunspots Increase Ionisation & Trigger X-Ray Flares
Magnetic Classification of Sunspots at 17.4 nm
Solar Terrestrial Activity Report
Real-Time
Sunspot Butterfly Diagram
EISN Estimated International Sunspot Number
Sunspot Number History &
Cycle Progression and ISES «Consensus» Forecast
10.7 cm Radio Flux Proxy of Ionisation
10.7 cm Radio Flux Progression
10.7 cm Radio Flux 27-Day Outlook10.7 cm Radio Flux USAF 45-Day ForecastSunspot &
HF Propagation OverviewTODO
Localised heliomagnetic field concentrations push away the Sun’s convection cells, revealing spots of the cooler photosphere below, called sunspots. Traces of iron in our Sun, produced by a previously exploded star, are concentrated in the strong magnetic fields of sunspots. Iron (Fe) plasma, more than anything else on the Sun, is what emits extreme UV radiation. Eight minutes later, this extreme UV radiation hits Earth’s ionosphere, significantly enhancing its ionisation.
Extreme UV from the Sun gets fully absorbed by Earth’s atmosphere. This and the fact that extreme UV mirrors are hard to build, render direct measurements of extreme UV flux impossible. Instead, proxies of extreme UV radiation are used, such as sunspot numbers and the 10.7 cm radio flux.
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