期刊
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
卷 54, 期 5, 页码 807-816出版社
OXFORD UNIV PRESS
DOI: 10.1093/pasj/54.5.807
关键词
line : profiles; Sun : corona; Sun : magnetic fields; techniques : spectroscopic
We have obtained spectrographic observations of several coronal regions in three emission lines (6374 Angstrom [Fe x], 10747 Angstrom [Fe XIII], and 10798 Angstrom [Fe X111]) simultaneously. The 25-cm coronagraph at Norikura Observatory and two large-format CCD cameras were used. The peak intensity, velocity, and line-width values were derived from Gaussian fits to the observed line profile at each location of the observed region. The ratio of the intensities of the 10747 Angstrom and 10798 Angstrom emission lines in the individual coronal structures range between 1.0 and 2.5 at 10 above the limb, which corresponds to a density range of 9.8 x 10(9)-2.4 x 10(8) cm(-3). The scale-height temperature values, derived from the variations of the intensity ratio with height above the limb for all individual coronal structures, range between 0.6 x 10(6) K and 8.3 x 10(6) K with a most frequent value around 1.8 x 10(6) K. The large values of the scale-height temperature for 70% of the structures indicate that these structures may not be in hydrostatic equilibrium nor be isothermal in nature.
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