The Electron Temperature of the Solar Transition Region

Details The Electron Temperature of the Solar Transition Region The Electron Temperature of the Solar Transition Region

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsp43c..05m&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SP43C-05

Physics

7507 Chromosphere, 7524 Magnetic Fields, 7546 Transition Region, 7549 Ultraviolet Emissions

Scientific paper

There are few spectroscopic measurements of electron temperature in the solar transition region (the temperature region from about 2×104 K to 8×105 K). This is because UV and EUV spectral lines from which temperature sensitive intensity ratios can be formed are usually far separated in wavelength and cannot be observed by a single instrument. Therefore, temperatures inferred for the transition region are usually obtained from experimentally untested theory that furthermore depends on the assumption of ionization equilibrium. However, between 30 March 2007 and 14 April 2007 there was a joint campaign between the SUMER spectrometer on SOHO and the EIS spectrometer on Hinode. The EIS spectrometer operates in two narrow wavelength bands: 170 — 210 and 250 — 290 Å. The SUMER spectrometer operates roughly between about 500 and 1610 Å. Both SUMER and EIS jointly observed portions of quiet Sun and active regions and obtained spectra that include lines from a number of the same transition region ions. The ratios of some of these lines from the same ion are temperature sensitive and provide an unprecedented opportunity to measure the temperatures of ion formation in the transition region and to compare these temperatures with the values obtained from theoretical ionization equilibrium calculations. A good example is the lines of O VI at 183.94, 184.12 Å (EIS) and 1031.92, 1037.61 Å (SUMER). We discuss temperatures derived for quiet Sun and active region transition regions from joint spectra obtained during the SUMER/EIS campaign.

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