Prominences and filaments are two manifestations of the same phenomenon. Both prominences and filaments are features formed above the chromosphere by cool dense gases held in place by solar magnetic fields. Filaments are observed on the solar disk as dark structures as seen against the hotter chromosphere whereas prominences on the limb appear bright against the perspective of outer space. The scale sizes for prominences and filaments are typically many thousands kilometers. Solar observers typically view prominences and filaments in Hydrogen alpha (656.3 nm). Filaments are sometimes referred to as floccule (plural of flocculus). Prominences and filaments can rapidly form over a period of a day but then typically persist for several weeks and, in some cases, several months. At breakup the gases within these previously stable structures may be explosively released into space in the form of a coronal mass ejection (CME). Space weather operators have and continue to monitor the location and character of prominences and filaments as potential precursors on near-earth geomagnetic activity. (Browse image provided courtesy of http://www.greatdreams.com)

A short-lived sudden increase in the intensity or radiation emitted in the neighborhood of sunspots monitored in H-alpha.

Collection includes a variety of indices related to solar activity contributed by a number of national and private solar observatories located worldwide. This metadata record is currently under construction.[SolarIndices A]

Collection includes a variety of indices related to solar activity contributed by a number of national and private solar observatories located worldwide. This metadata record is currently under construction.[SolarIndices A]

Collection includes a variety of indices related to solar activity contributed by a number of national and private solar observatories located worldwide. This metadata record is currently under construction.[SolarIndices A]

The GOES Solar X-ray Imager is integrated into the GOES-12 satellite, whose primary mission is to provide Earth-weather monitoring. The SXI is operated by NOAA's National Environmental Satellite, Data, and Information Service (NESDIS). NOAA's Space Environment Center (SEC) receives the telemetry stream directly from SXI, processes the data, and integrates the observations into their space weather alert and forecast services. The data are sent in real time to NOAA National Centers for Environmental Information (formerly National Geophysical Data Center) where they are immediately made available to the public, and preserved in a secure archive for future research. SXi was launched in with GOES-M on July 23, 2001 Post Launch Test data were available from August - December 2001.SXI officially entered operations in April 2003.

Solar x-ray flux data.

This archived Paleoclimatology Study is available from the NOAA National Centers for Environmental Information (NCEI), under the World Data Service (WDS) for Paleoclimatology. The associated NCEI study type is Forcing. The data include parameters of climate forcing with a geographic location of Global. The time period coverage is from 3095 to 5 in calendar years before present (BP). See metadata information for parameter and study location details. Please cite this study when using the data.

This archived Paleoclimatology Study is available from the NOAA National Centers for Environmental Information (NCEI), under the World Data Service (WDS) for Paleoclimatology. The associated NCEI study type is Forcing. The data include parameters of climate forcing with a geographic location of Global. The time period coverage is from 340 to -50 in calendar years before present (BP). See metadata information for parameter and study location details. Please cite this study when using the data.

Solid state detectors with pulse height discrimination measure proton, alpha-particle, and electron fluxes. E1 and I1 channels are responding primarily to trapped outer-zone particles. The I2 channel may occasionally respond to trapped particles during magnetically disturbed conditions. The remaining proton integrals measure fluxes originating outside the magnetosphere from the Sun or the heart of the Galaxy.Users of GOES particle data should be aware that significant secondary responses may exist in the particle data, i.e. responses from other particles and energies and from directions outside the nominal detector entrance aperture. The integrated protons displayed in these plots have been partially corrected for these effects. The electron detector responds significantly to protons above 32 MeV. Electron plots from GOES-8 to GOES-12 use data that have been corrected for this, earlier plots use uncorrected data. All electron data become unreliable during ion storms.