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Magnesium emission variability among late-type giant stars
Profiles of the Mg II h and k emission features in the spectra of 21late-type giant stars were obtained. Emission strengths were separatelymeasured in the shortward (S) and longward (L) components. Variations intotal emission intensity (S + L) can be interpreted as evidence forvariations in the rate of mechanical energy deposition in thechromosphere. Mass loss processes in the corona/outer atmosphere may bestrong enough to affect the ratio of S/L: thus, rapid mass loss causesS/L to be less than unity. Rapid mass loss is likely caused bydeposition of mechanical energy by stellar wind. Variations in S/L are ameasure of variations in the rate of mechanical energy deposition in thecorona/outer atmosphere. The stellar sample variations were divided intofour classes: (1) variations in S/L; (2) variations in the circumstellarabsorption components; (3) variations in the total flux; and (4) noevidence for variations found on the time scales used.
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| Takýmyýldýz: | Kanatli At |
| Sað Açýklýk: | 21h42m51.79s |
| Yükselim: | +10°30'42.8" |
| Görünürdeki Parlaklýk: | 9.292 |
| özdevim Sað Açýklýk: | 1 |
| özdevim Yükselim: | -6.9 |
| B-T magnitude: | 9.697 |
| V-T magnitude: | 9.326 |
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