A coronal mass ejection (or CME) is a giant cloud of solar plasma drenched with magnetic field lines that are blown away from the Sun during strong, long-duration solar flares and filament eruptions. The first proof of these dynamic events came from observations made with a coronagraph on the OSO 7 spacecraft between 1971 and 1973. A coronagraph produces a solar eclipse by covering the Sun with a small disk. Coronal mass ejections are very faint and can not be observed otherwise. The SOHO and STEREO missions have white-light coronagraphs onboard to detect coronal mass ejections. coronal mass ejections are the prime source of strong geomagnetic storms and thus very important to keep an eye on. The animation below shows a coronal mass ejection as seen by LASCO onboard the SOHO spacecraft.
A coronal mass ejection can escape from the Sun during eruptions on the Sun like solar flares and filament eruptions. However, not every event has a coronal mass ejection accompanied with it. Strong flares (M and X-class) are likely candidates to launch coronal mass ejections. C-class solar flares can also produce coronal mass ejections but only the long-duration and stronger C-class flares might do this. It also depends on the duration of the solar flare. For example, when there is a solar flare with a peak strength of X5 and with a total duration of two hours then it will certainly be accompanied with a bright, large and fast coronal mass ejection. Depending on the location of the eruption, the blast could either miss Earth, be partially or fully Earth-directed. An Earth-directed coronal mass ejection will look like a partial or full-halo coronal mass ejection on the images from SOHO. When this happens the coronal mass ejection will arrive at Earth after 24 hours or more (depending on the speed) and will likely cause a geomagnetic storm with vivid auroral displays. The animation below shows a full halo coronal mass ejection as seen by SOHO/LASCO.
When the Sun isn't very active during solar minimum, coronal mass ejections are rare. There might only be one coronal mass ejection every week. When the Sun's activity increases towards solar maximum, coronal mass ejections become more common and we can see multiple coronal mass ejections every day.
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|M-class solar flare||1%|
|X-class solar flare||1%|
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|Last geomagnetic storm:||2017/02/01||Kp5 (G1)|
|Number of spotless days in 2017:||11|
|Current stretch spotless days:||2|