Solar wind speed and He I (1083 nm) absorption line intensity

Details Solar wind speed and He I (1083 nm) absorption line intensity Solar wind speed and He I (1083 nm) absorption line intensity

Apr 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991jgr....96.5397h&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 96, April 1, 1991, p. 5397-5403.

Physics

8

Absorption Spectra, Helium Ions, Magnetic Field Configurations, Scintillation, Solar Wind Velocity, Chromosphere, Coronal Holes, Interplanetary Magnetic Fields, Photosphere, Solar Rotation

Scientific paper

An attempt is made to identify regions in the photosphere from which solar winds originate using the interplanetary scintillation (IPS) method. Values of the solar wind speed estimated by IPS observations are projected onto a spherical surface of 2.5 solar radii. The data during five Carrington rotations in 1984 are superimposed on this 'source surface' to construct an average map of the solar wind speed distribution. This distribution is then projected onto the photosphere along the coronal magnetic field lines. It is found that there is a linear relation between the solar wind speeds and intensities of the He I absorption line at corresponding locations on the chromosphere. Since the intensity of this line is coupled with the coronal temperature, this relation suggests that some physical mechanism in or above the photosphere accelerates coronal plasmas to the solar wind speed in regions where the temperature is low. It is suggested that the efficiency of the acceleration decreases as coronal temperature increases.

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