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Glossary term: K 型星

Description: 光譜類型為 ”K“ 的恆星。天文學家通過光譜中氫原子譜線非常弱但鐵和錳原子譜線較強來識別 K 型星。它們的典型(有效)溫度大約在 3700 K 到 5200 K 之間。與其他恆星相比,它們在人眼中呈現橙白色,除非受到星際或大氣層紅化的影響。金牛座的畢宿五(即阿爾德巴朗)和雙子座的北河三(即波魯克斯)就是 K 型星。

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Term and definition status: The original definition of this term in English have been approved by a research astronomer and a teacher
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This is an automated transliteration of the simplified Chinese translation of this term

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Related Diagrams


A ragged line peaking about 580 nm then declining at longer wavelengths with a few deeper dips.

Spectrum of a K-type star

Caption: The spectrum of the K-type star 2MASS J19554455+4754531. The colour of the line between 400 nm and 700 nm roughly corresponds to the colour the human eye would see light of that wavelength. Below 400 nm and above 700 nm, where the human eye can see little to no light, the lines are coloured blue and red respectively. The black lines show spectral absorption lines caused by atoms and ions of different elements in the star’s atmosphere. These atoms and ions absorb at specific wavelengths, causing sharp, dark lines in the spectra. How strong these lines are depends on the temperature of the star’s atmosphere. Two stars made from the same mix of elements could have spectra with vastly different sets of lines in their spectra if they have different temperatures in their atmospheres. The spectra of K-type stars are dominated by metal atoms such as iron, sodium and calcium atoms. There are so many lines from metal atoms, far too many to mark individually, that the spectrum has a choppy, ragged appearance. The lines of hydrogen atoms and calcium ions are much weaker than in the hotter G-type stars.
Credit: IAU OAE/SDSS/Niall Deacon

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