Redshifts of high-temperature emission lines in the far-ultraviolet spectra of late-type stars

Details Redshifts of high-temperature emission lines in the far-ultraviolet spectra of late-type stars Redshifts of high-temperature emission lines in the far-ultraviolet spectra of late-type stars

Nov 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...274..801a&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 274, Nov. 15, 1983, p. 801-814.

Astronomy and Astrophysics

Astronomy

60

Emission Spectra, Far Ultraviolet Radiation, High Temperature, Late Stars, Line Spectra, Red Shift, Iue, Optical Thickness, Solar Activity, Solar Magnetic Field, Spaceborne Astronomy, Stellar Winds, Ultraviolet Spectra

Scientific paper

High-dispersion IUE spectra of six late-type stars exhibit small but statistically significant differential redshifts of high-temperature emission lines, like Si IV and C IV, with respect to low-temperature lines like S I and O I. A well-exposed, small-aperture spectrum of the active chromosphere binary Capella (Alpha Aurigae A: G6 II+F9 III) establishes that the high-temperature lines are redshifted in an absolute sense with respect to the accurately determined photospheric velocity of the system at single-line phase 0.50. Several possible explanations for the stellar redshifts are discused, including a warm wind (100,000 K) in which aparent redshifts are produced in optically thick lines by an accelerating outfow, and the downflowing component of a vertical circulation system for which the up-leg portion of the flow is too cool, too hot, or too tenuous to be visible in Si IV and C IV. If the second scenario is true, the stellar redshifts may provide an important phenomenological link to the downflows observed in 100,000 K species over magnetic active regions in the sun.

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