On the Detection of Solar Coronal High-Velocity Fields Using the XUV Doppler Telescope

Details On the Detection of Solar Coronal High-Velocity Fields Using the XUV Doppler Telescope On the Detection of Solar Coronal High-Velocity Fields Using the XUV Doppler Telescope

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000pasj...52.1165k&link_type=abstract

Publications of the Astronomical Society of Japan, v.52, p.1165-L1174.

Astronomy and Astrophysics

Astronomy

1

Sun: Atmospheric Motions, Sun: Corona, Sun: X-Rays

Scientific paper

The XUV Doppler Telescope (XDT) is a sounding rocket experiment designed to detect flows in the solar corona using filter ratios. The XDT, successfully launched on 1998 January 31, is a normal incidence telescope composed of narrow-bandpass multilayer mirrors and capable of obtaining images 2 Å\ above and 2 Å\ below the Fe XIV 211 Å\ (T = 1.7 MK) emission line. It has the potential to make a velocity map of the entire solar disk with just a few minutes of observation. The image ratio maps show features that translate to Doppler shifts of 200 km s-1 or more, including several `redshift' features located near footpoints of coronal loops. However, no corresponding velocity features were seen by the Solar and Heliospheric Observatory (SOHO) Coronal Diagnostic Spectrometer (CDS) in the Mg IX 368 Å (T = 1 MK) line, suggesting that the features are not caused by Doppler shift. Instead, the features seem to be related to contamination of lower temperature (T < 1 MK) emission lines and the nearby density-sensitive Fe XIII lines. We conclude that while no flows were positively identified by the XDT, this observing technique is capable of detecting flows of 1000 km s^{-1} independently, and 200 km s^{-1}$ when combined with simultaneous plasma diagnostic observation.

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