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    Space Weather Observations, Alerts, and Forecast

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    CloudFront

    Sun Images


    eit 171 eit 195 eit 284 eit 304
     

    Images: From left to right: EIT 171, EIT 195, EIT 284, EIT 304 EIT (Extreme ultraviolet Imaging Telescope) images the solar atmosphere at several wavelengths, and therefore, shows solar material at different temperatures. In the images taken at 304 Angstrom the bright material is at 60,000 to 80,000 degrees Kelvin. In those taken at 171 Angstrom, at 1 million degrees. 195 Angstrom images correspond to about 1.5 million Kelvin, 284 Angstrom to 2 million degrees. The hotter the temperature, the higher you look in the solar atmosphere.

     
    SDO/HMI
    Continuum
    SDO/HMI
    Magnetogram
    LASCO C2 LASCO C3
     

    The MDI (Michelson Doppler Imager) images shown here are taken in the continuum near the Ni I 6768 Angstrom line. The most prominent features are the sun spots.
     

    LASCO (Large Angle Spectrometric Coronagraph) is able to take images of the solar corona by blocking the light coming directly from the Sun with an occulter disk, creating an artificial eclipse within the instrument itself.

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    Solar cycle


    Sunspot numbers F10.7CM Radio flux AP
     
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    The Solar Cycle is observed by counting the frequency and placement of sunspots visible on the Sun. Solar minimum occurred in December, 2008. Solar maximum in May, 2013.

     
    Solar wind Satellite impact Xray flux
     
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    On the left: Real-Time Solar Wind data broadcast from NASA's ACE satellite. Middle: The Satellite Environment Plot combines satellite and ground-based data to provide an overview of the current geosynchronous satellite environment. Right: 3-days of 5-minute solar x-ray flux values measured on the SWPC primary and secondary GOES satellites.

    Auroral activity


    Northern Auroral map Southern Auroral map
     

    Instruments on board the NOAA Polar-orbiting Operational Environmental Satellite (POES) continually monitor the power flux carried by the protons and electrons that produce aurora in the atmosphere. SWPC has developed a technique that uses the power flux observations obtained during a single pass of the satellite over a polar region (which takes about 25 minutes) to estimate the total power deposited in an entire polar region by these auroral particles. The power input estimate is converted to an auroral activity index that ranges from 1 to 10.

    Introduction Movie


    Conditions on the Sun and in the solar wind, magnetosphere, ionosphere and thermosphere that can influence the performance and reliability of space-borne and ground-based technological systems and can endanger human life or health. This introduction movie in the English language will open on a new tab/window when you click on the image below.



    Also in Quicktime format: Large (269M) and Small ( 60M).


    Credits:

    Space Weather Images and Information (excluded from copyright) courtesy of:
    NOAA / NWS Space Weather Prediction Center, Mauna Loa Solar Observatory (HAO/NCAR), and SOHO (ESA & NASA).

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