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The current time is: 17:14 UTC on Monday, March 28, 2005
Solar Wind Data
WWV only updates its SFI reading once a day at 2100Z The Penticton solar observatory takes measurements at 1700Z, 2000Z, and 2300Z (WWV uses the 2000Z Penticton measurement)
(updated daily after 2200Z)
(usually reported within 30 minutes of event peak)
This number is reported daily around 2025Z and reports the number of sunspots observed in the previous 24 hour period
This value is reported daily around 2025Z and reports the average background x-ray flux level as measured by the GOES-8 satellite
Auroral Activity Aurora (also known as "aurora borealis" or "northern lights") is caused by interaction between the Earth's magnetic field and the solar wind (a mix of charged particles blowing away from the sun). During solar storms, enough of these charged particles make it through to the Earth's upper atmosphere that they interact with the earths natural magnetic field lines. When enough of these particles collide, energy is released in the form of auroral light. In addition to creating a pretty light show (mostly in upper latitudes), radio signals scatter off of these particles and can greatly enhance propagation on 6 meters and above. High levels of aurora can also make HF propagation via polar routes difficult. Click on thumbnails to
view a larger image مستوى الأشعة السينية Solar X-ray Flux This chart shows X-ray flux levels as measured by the GOES-8 and GOES-10 satellites. The GOES-8 measurements (shown in red) are used to issue "solar alerts" when X-ray flux levels exceed certain levels. Spikes on the chart correspond to solar flares. Flares are considered "significant" when flux levels rise above the "M" level (as shown on the right side of the chart). These large flares can often wipe out the ham radio and shortwave bands almost immediately and it can take minutes to hours for the bands to recover. If the bands seem to go dead all of a sudden, it is always a good idea to check this chart to see if a large flare has occurred recently. Dynamically updating
plots: خريطة أعلى متسوى للموجات الصالحة للإتصال Near-Real-Time MUF map The following map shows Maximum Usable Frequencies (MUFs) for 3000 kilometer radio signal paths. More importantly, the current sunspot number (SSN) and Planetary A-index are updated every 30 minutes on the bottom of this image. Additionally, the grey line position, auroral ovals, and sun position are provided. Click on the map for more details on how to use it. This image courtesy of Solar Terrestrial Dispatch صور حيّة للشمس Current Solar Images The images below are current views of the sun shown at different wavelengths of light as taken by SOHO and the Yohkoh soft-Xray telescope. Generally, more bright regions on the disk indicates more solar activity, which usually leads to higher solar flux levels (which also often leads to better ham radio and shortwave propagation!). Click on any thumbnail to view a larger image. Sometimes you may see the text "CCD Bakeout" instead of the solar disc images. This occurs when NASA does routine maintenance and calibration on the cameras. For a more technical explanation, read NASA CCD Bakeout explanation. Images courtesy of the Solar Data Analysis Center at the NASA Goddard Space Flight Center |
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جميع الحقوق محفوظة. تصميم و تنفيذ شركة نازا - لبنان. Copyright © NASACO |
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