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The infrared Ca II triplet, commonly known as the calcium triplet, is a set of three ionized calcium spectral lines at the wavelengths of 8498 Å, 8542 Å and 8662 Å (measured in air). The triplet is most often observed in absorption in the spectra of stars of spectral type G, K and M.[1][2][3] Some Be stars, which are hot stars with hydrogen emission lines, show the calcium triplet in emission. [4] The emission seems to come from peculiar properties of the gas disk that surrounds the star and produces the hydrogen emission lines. [5]
See also
[edit]References
[edit]- ↑ Andretta; Busà; Gomez; Terranegra (2005). "The Ca II Infrared Triplet as a stellar activity diagnostic" (PDF). Astronomy & Astrophysics. p. 669.
- ↑ Jonathan Tennyson (2005). "Astronomical Spectroscopy. An introduction to the atomic and molecular physics in astronomical spectra" (PDF). Imperial College Press. p. 94. Archived from the original (PDF) on 2016-01-16. Retrieved 2016-07-09.
- ↑ G. Kordopatis, A. Recio-Blanco, P. de Laverny, A. Bijaoui, V. Hill, G. Gilmore, R. F. G. Wyse and C. Ordenovic (2011). "Automatic stellar spectra parameterisation in the IR Ca ii triplet region" (PDF). Astronomy & Astrophysics. p. 535, A106. Archived from the original on 2011-11-21.
{{cite web}}: CS1 maint: multiple names: authors list (link) - ↑ Polidan, R. S.; et al. (1976). "On the Detection of Binary be Stars" (PDF). Be and Shell Stars: IAU Symposium No. 70. 70: 405. Bibcode:1976IAUS...70..401P.
- ↑ Koubský, Pavel; et al. (2012). "Calcium Emission in Interacting Binary Be Stars". arXiv:1205.2259 [astro-ph.SR].
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