Space Weather on 21 April 2024, 10:21 UTC

 
SN 220 | SFI 210 | Kp 3 | Ap 14 | Kt 3 | At 27 | Bz -4.2 | Dst -34 | XRY 1.00 | Pf 0.2 | SW 451

Sunspot Numbers for VOACAP

The SSN source of (near-)current sunspot numbers to be used with VOACAP: SIDC (Belgium).


Real-Time K-Index

A 3-hourly index of geomagnetic activity expressed in the logarithmic units on a scale from 0 to 9.



Source: https://flux.phys.uit.no/Kindice/k_tro2a.gif (Tromso Geophysical Observatory)


Magnetogram: State of Earth's Magnetic Field

Variations in Earth's magnetic field are measured by magnetometers. Any strong and sudden variations (up or down) in the X component (uppermost graph) are indications of VHF radio-auroral activity (e.g. on 144 MHz when variations suddenly peak, say, 300 nT).

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Source: https://www.sgo.fi/Data/RealTime/Kuvat/magrtday.png (Sodankylä Geophysical Observatory)




Source: https://flux.phys.uit.no/Last24/Last24_kev1a.gif, (Utsjoki/Kevo)


Real-Time Solar Wind



Source: https://services.swpc.noaa.gov/images/ace-mag-swepam-3-day.gif (NOAA, Space Environment Prediction Center)


Solar X-Ray Flux

Class M and X flares affect the sunlit area of the Earth, causing increased D-region absorption. Strong flares are source of Shortwave Fadeouts (SWF) and Sudden Ionospheric Disturbances (SID).

See GOES X-Ray Flux (NOAA Space Weather Prediction Center)


Solar Proton Flux

High-energy protons are guided into the polar cap by Earth's magnetic field. Strong proton bursts are source of Polar Cap Absorption (PCA), i.e. high D-region absorption on paths passing through the polar areas.

See GOES Proton Flux (NOAA Space Weather Prediction Center)



Source: https://services.swpc.noaa.gov/images/swx-overview-small.gif