Magnesium emission variability among late-type giant stars

Details Magnesium emission variability among late-type giant stars Magnesium emission variability among late-type giant stars

Feb 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...253..716m&link_type=abstract

Astrophysical Journal, Part 1, vol. 253, Feb. 15, 1982, p. 716-726.

Astronomy and Astrophysics

Astrophysics

19

Emission Spectra, Giant Stars, Late Stars, Magnesium, Stellar Spectra, Variability, Atmospheric Heating, Chromosphere, High Resolution, Iue, Line Spectra, Periodic Variations, Radiant Flux Density, Spectral Resolution, Stellar Spectrophotometry, Stellar Structure, Ultraviolet Spectra

Scientific paper

Profiles of the Mg II h and k emission features in the spectra of 21 late-type giant stars were obtained. Emission strengths were separately measured in the shortward (S) and longward (L) components. Variations in total emission intensity (S + L) can be interpreted as evidence for variations in the rate of mechanical energy deposition in the chromosphere. Mass loss processes in the corona/outer atmosphere may be strong enough to affect the ratio of S/L: thus, rapid mass loss causes S/L to be less than unity. Rapid mass loss is likely caused by deposition of mechanical energy by stellar wind. Variations in S/L are a measure of variations in the rate of mechanical energy deposition in the corona/outer atmosphere. The stellar sample variations were divided into four classes: (1) variations in S/L; (2) variations in the circumstellar absorption components; (3) variations in the total flux; and (4) no evidence for variations found on the time scales used.

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