Further observations of the 10830-A helium line in stars and their significance as a measure of stellar activity

Details Further observations of the 10830-A helium line in stars and their significance as a measure of stellar activity Further observations of the 10830-A helium line in stars and their significance as a measure of stellar activity

Sep 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976apj...208..414z&link_type=abstract

Astrophysical Journal, vol. 208, Sept. 1, 1976, pt. 1, p. 414-425.

Other

76

Emission Spectra, Helium, Late Stars, Stellar Spectra, Astronomical Catalogs, Chromosphere, Coronas, F Stars, K Lines, K Stars, Statistical Analysis, Variable Stars

Scientific paper

Measurements of the 10830-A He line in 198 stars are given along with data on other features in that spectral range. Nearly 80 per cent of all G and K stars show some 10830-A absorption or emission; of these, half are variable and one-quarter show emission. The results of Vaughan and Zirin (1968) are confirmed that the 10830-A line is not found in M stars, is weak in F stars, and is particularly strong in close binaries. The line is found in emission in extremely late M and S stars along with P-gamma, but the latter is not in emission in the G and K stars with 10830-A emissions. Variable He emission along with Ti I emission is found in the RV Tauri variables R Sct and U Mon. In R Aqr, the Fe XIII coronal line at 10747 A is found in emission along with a line at 11012 A, which may be singlet He or La II, as well as the 10830-A and P-gamma lines. There is possibly a five-year period in the appearance of 10830-A emission in theta Her. The nature of coronae or hot chromospheres in the various stars is extensively discussed without definite conclusion, except that the 10830-A intensity must be more or less proportional to the energy deposited in the chromosphere-corona by nonthermal processes.

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