EUV Spectral Line Profiles in Polar Coronal Holes from 1.3 to 3.0 R_solar

Details EUV Spectral Line Profiles in Polar Coronal Holes from 1.3 to 3.0 R_solar EUV Spectral Line Profiles in Polar Coronal Holes from 1.3 to 3.0 R_solar

Jan 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999apj...510l..59k&link_type=abstract

The Astrophysical Journal, Volume 510, Issue 1, pp. L59-L62.

Astronomy and Astrophysics

Astronomy

83

Line: Profiles, Sun: Solar Wind, Sun: Corona, Sun: Uv Radiation

Scientific paper

Spectral line profiles have been measured for H I lambda1216, O VI lambdalambda1032, 1037, and Mg X lambda625 in a polar coronal hole observed during 1997 September 15-29, at projected heliographic heights rho between 1.34 and 2.0 R_solar. Observations of H I lambda1216 and the O VI doublet from 1997 January for rho=1.5-3.0 R_solar are provided for comparison. The O VI lines are well fit to a narrow and broad component which appear to be associated with regions of higher and lower spectral radiance, respectively. The narrow components dominate at low heights and become a small fraction of the lines at higher heights. Mg X lambda625 is observed to have a narrow component at rho=1.34 R_solar which accounts for only a small fraction of the observed spectral radiance. In the case of the broad components, the values of v_1/e for O VI are only slightly larger than those for H I at rho=1.34 R_solar but are significantly larger at rho=1.5 R_solar and much larger for rho>1.75 R_solar. In contrast, the Mg X values are less than those of H I up to 1.75 and then increase rapidly up to at least rho=2.0 R_solar but never reach the values of O VI.

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