Solar wind & Earth magnetosphere data to support 160m propagation observations

Below comments (like, "less is better") are meant for low band HF propagation. Not for VHF, and not for aurora visual observers, in which case it is basically the opposite

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You can zoom into specific time frame of the graph using mouse (left-click&hold/select range/release).

Last 24 hours

Less is better. Red dots: Bz<0 (bad for polar paths); Blue dots: Bz>0;

Positive Bz is better and most important for polar paths.

Less is better for polar paths & high latitudes

Last 7 days

Less is better. Red dots: Bz<0 (bad for polar paths); Blue dots: Bz>0;

Positive Bz is better and most important for polar paths.

Less is better for polar paths & high latitudes

(in the above graph more nT means less disturbed magnetosphere. Close to 0 or above 0 should be good for polar paths on topband)

In the case of a classic magnetic storm, the Dst shows a sudden rise, corresponding to the storm sudden commencement, and then decreases sharply as the ring current intensifies. Once the IMF turns northward again and the ring current begins to recover, the Dst begins a slow rise back to its quiet time level

About DST index

Peaks indicate Solar flares. After 8 minutes a (big) flare can cause radio blackouts, after 20 minutes - solar radiation storm, after 2-4 days - if and when released coronal mass ejection hits Earth it may cause a geomagnetic storm

Less is better for 160m band propagation (<100). More is better for 20m and higher bands (>100)

About 10.7 cm flux

Separate page with Proton and Electron flux data

This separate page plots data showing Proton and Electron flux data from GOES geostationary satellites

Magnetometer stacked data (North on top, South on bottom)

Europe

North America

Data sources:

Mostly different observation products of SWPC
https://www.swpc.noaa.gov/products/real-time-solar-wind
https://www.swpc.noaa.gov/products/aurora-30-minute-forecast
https://services.swpc.noaa.gov/products/kyoto-dst.json https://www.swpc.noaa.gov/products/goes-x-ray-flux

Also: http://flux.phys.uit.no/stackplot/

Some FAQ on Space weather topics: NASA FAQ

About hemispheric Power

The OVATION model calculates a globally integrated total energy deposition in GigaWatts 30 to 90 minutes in the future. The forecast lead time is the time it takes for the solar wind to travel from the L1 observation point to Earth. For values below about 20GW, there may be little or no aurora observable. For values between 20 and 50, you may need to be near the aurora to see it. For values above 50, the aurora should be quite observable with lots of activity and motion across the sky. Once the Hemispheric Power reaches levels of 100 or more, this is considered to be a very significant geomagnetic storm
Source: https://www.swpc.noaa.gov/products/aurora-30-minute-forecast
https://www.spaceweatherlive.com/en/auroral-activity/auroral-oval

Page created by YL2VW for self education and HF, mainly 160m band, propogation study purposes