XUV Photometer System (XPS): Solar Variations during the SORCE Mission

Details XUV Photometer System (XPS): Solar Variations during the SORCE Mission XUV Photometer System (XPS): Solar Variations during the SORCE Mission

Aug 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005soph..230..375w&link_type=abstract

Solar Physics, Volume 230, Issue 1-2, pp. 375-387

Physics

17

Scientific paper

The solar soft X-ray (XUV) radiation is important for upper atmosphere studies as it is one of the primary energy inputs and is highly variable. The XUV Photometer System (XPS) aboard the Solar Radiation and Climate Experiment (SORCE) has been measuring the solar XUV irradiance since March 2003 with a time cadence of 10 s and with about 70% duty cycle. The XPS measurements are between 0.1 and 34 nm and additionally the bright hydrogen emission at 121.6 nm. The XUV radiation varies by a factor of ˜2 with a period of ˜27 days that is due to the modulation of the active regions on the rotating Sun. The SORCE mission has observed over 20 solar rotations during the declining phase of solar cycle 23. The solar XUV irradiance also varies by more than a factor of 10 during the large X-class flares observed during the May June 2003, October November 2003, and July 2004 solar storm periods. There were 7 large X-class flares during the May June 2003 storm period, 11 X-class flares during the October November 2003 storm period, and 6 X-class flares during the July 2004 storm period. The X28 flare on 4 November 2003 is the largest flare since GOES began its solar X-ray measurements in 1976. The XUV variations during the X-class flares are as large as the expected solar cycle variations.

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