UV and Soft X-ray Polar Coronal Jets

Details UV and Soft X-ray Polar Coronal Jets UV and Soft X-ray Polar Coronal Jets

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mwoc.conf...23d&link_type=abstract

Multi-Wavelength Observations of Coronal Structure and Dynamics -- Yohkoh 10th Anniversary Meeting. Proceedings of the conferenc

Astronomy and Astrophysics

Astrophysics

Scientific paper

Coronal jets are spectacular dynamic events originating from different structures in the solar corona. Jetlike phenomena were observed by various instruments aboard SOHO, and the X--ray jets were discovered by Yohkoh's soft X--ray telescope (SXT). The relation among the different types of jets is still not yet clear. We present ultraviolet spectroscopy of polar coronal jets obtained by the Ultraviolet Coronagraph Spectrometer (UVCS/SOHO) at heights in the corona ranging from 1.5 Rodot to 2.5 Rodot. The jets appear to originate near flaring ultraviolet bright points within polar coronal holes and were recorded by UVCS as a significant enhancement in the integrated intensities of the strongest coronal emission lines: mainly H I Ly alpha and O VI lambda lambda 1032,1037. A number of the detected jets are correlated with EIT Fe XII 195Å and LASCO C2 white-light events. Our modeling of the jet's observable properties provided estimates of the jet plasma conditions, as well as the initial electron temperature and heating rate required to reproduce the observed O VI ionization state. We discuss possible relationship between the polar ultraviolet and X--ray jets based on the results of coordinated SXT and UVCS observations in December 1996. We compare their properties and consider the magnetic reconnection models, developed for X--ray jets, as a model for UV jet formation. This work is supported by the National Aeronautics and Space Administration under grant NAG5--10093 to the Smithsonian Astrophysical Observatory, by Agenzia Spaziale Italiana, and by the ESA PRODEX program (Swiss contribution).

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