![]() The menu also offers the ability to download the displayed numerical data in JSON format. The dynamic plot above can be downloaded in multiple image formats using the menu at the upper right. Sometimes the algorithm will not trigger on a flare with a gradual rise-time (common for limb events), and the forecaster will have to enter the particulars manually. The end time is the time when the flux level decays to a point halfway between the maximum flux and the pre-flare background level.The X-ray event maximum is taken as the minute of the peak X-ray flux.The begin time of an X-ray event is defined as the first minute, in a sequence of 4 minutes, of steep monotonic increase in 0.1-0.8 nm flux.The particulars for defining the begin, maximum, and end-time of an X-ray event are: The latest event is the latest X-ray flare detected by the GOES satellites, either automatically or manually entered if the detection algorithm fails, without regard to any earlier events. Some large flares are accompanied by strong radio bursts that may interfere with other radio frequencies and cause problems for satellite communication and radio navigation (GPS). SWPC sends out space weather alerts at the M5 (5x10 -5 Watts/mw) level. Solar flares are also associated with Coronal Mass Ejections (CMEs) which can ultimately lead to geomagnetic storms. 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. ![]() The GOES X-ray plots shown here are used to track solar activity and solar flares.
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