TIMED SEE News
The composite Lyman-alpha time series has been updated to include the latest versions of the TIMED SEE and SORCE SOLSTICE solar irradiance measurements of the bright H I 121.5 nm emission. These TIMED and SORCE data are used in the 2003-present time range and are scaled to match the UARS reference level as discussed by Woods et al. [JGR, 2000]. The composite time series goes back to 1947 using a combination of measurements and modeling results, all referenced to the UARS reference level.
In addition to the new TIMED and SORCE data, the composite Lyman-alpha time series has been updated in the 2001-2003 time frame with just model results. There are some measurements during that time from UARS and TIMED, but degradation issues for both of those instruments in the 2001-2003 time period need to be addressed first.
SEE Occultation Data Product Released. A new product containing atmospheric transmissions is now available for download via anonymous FTP. This one netcdf file contains the entire set of occultation data for the mission. Transmission measurements made by the TIMED-SEE EGS instrument range from 27-194 nm. The occultation data page has more details. Users are encouraged to view the README file.
SEE Flare Catalog Released. (Release information in PDF) The first version of the TIMED SEE flare catalog has been released and can be found at http://lasp.colorado.edu/see/see_flare_catalog.html. This catalog lists the solar flares that TIMED SEE has observed so far over its 6 years on orbit. Due to SEE's three percent duty cycle (only three minutes of observations every 96-minute orbit), it was originally expected that SEE would only observe about 1-2 GOES X-Class flares per year. SEE actually has measured the irradiance change for almost 100 flares to date, including observations during both the impulsive and gradual phases of the flares. SEE provides unique flare measurements over the entire vacuum ultraviolet (VUV) range from 0.1-193 nm at once, giving a complete spectral picture of the simultaneous increases of emissions formed throughout the solar atmosphere. These emissions range from the hot coronal X-ray ultraviolet (XUV, 0.1-10 nm), to the extreme ultraviolet (EUV, 10-120 nm) emissions that come from the cool corona and transition region, to the far ultraviolet (FUV, 121-193 nm) which are formed mainly in the chromosphere and upper photosphere.
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