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MB MPEG movie from the SOHO/LASCO instrument showing a month of CMEs fromĮjections: Observations by David F. Near solar maximum we observe an average of 2 to 3 CMEs per day The frequency of CMEs varies withĪt solar minimum we observe about one CME a week. As they loom larger and larger they appear to envelope the SunĬoronal mass ejections are often associated withįlares and prominence eruptions but they canĪlso occur in the absence of either of these processes. Halo events are produced by CMEs that areĭirected toward the Earth. It produced a "halo event" in which theĮntire Sun appeared to be surrounded by the CME. The event of April 7th, 1997 is shown to the left On the Solar and Heliospheric Observatory ( SOHO) TheĪnimated sequence of images at the top of this page were obtained with the High Altitude Observatory's coronagraph on the Solar Maximum Mission in April of 1980.Ĭoronal Mass Ejections disrupt the flow of the solar wind and produceĭisturbances that strike the Earth with sometimes catastrophic results. From space theĬorona is visible out to large distances from the Sun and can be viewed continuously. Only the innermost corona is visible above the brightness of the sky. The corona is only visible for a few minutes at most, too short a period of time to noticeĪny changes in coronal features. "occulting disk" over the image of the Sun. A coronagraph produces an artificial eclipse of the Sun by placing an Observations made with a coronagraph on the 7th Orbiting Solar Observatory (OSO 7) fromġ971 to 1973. The earliest evidence of these dynamical events came from Of the Sun for thousands of years, the existence of coronal mass ejections was unrealized Magnetic field lines that are ejected from the Sun over the course of several hours.Īlthough the Sun's corona has been observed during total eclipses Marshall Grazing Incidence X-ray Spectrometer (MaGIXS)Ĭoronal mass ejections (or CMEs) are huge bubbles of gas threaded with
Chromospheric Lyman-Alpha Spectro Polarimeter (CLASP)
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