Velocity fields in a low-latitude coronal hole - Results from the Solar Maximum Mission

Details Velocity fields in a low-latitude coronal hole - Results from the Solar Maximum Mission Velocity fields in a low-latitude coronal hole - Results from the Solar Maximum Mission

Jun 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...317..487m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 317, June 1, 1987, p. 487-501.

Other

5

Coronal Holes, Solar Maximum Mission, Spatial Distribution, Stellar Spectrophotometry, Ultraviolet Spectra, Velocity Distribution, Astronomical Maps, Atmospheric Circulation, Solar Atmosphere

Scientific paper

The Solar Maximum Mission (SMM) satellite has been used to observe Doppler signatures in C IV in a low-latitude coronal hole as it crossed the central meridian (1985 February 2-8). Scatter plots of C IV emission intensity versus velocity do not show the pronounced positive correlation which has been reported in other regions on the sun. These data suggest that the coronal hole may control the gross velocity field in the solar atmosphere at the level where C IV is formed. Some localized regions of upflow coincide with EUV bright points in the coronal hole.

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