Quantum redactiones paginae "Classis spectralis" differant

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Summarium vacuum
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== Introductio ==
== Classificatio Harvardiana ==
[[Imago:Morgan-Keenan spectral classification.png|500px|right|thumb|Classificatio Harvardiana]]
Classificatione Harvardiana, stellae dividuntur in classes O—B—A—F—G—K—M—C—S. Plerumque communes sunt stellae classium O—B—A—F—G—K—M, quae appellantur "stellae normales," sed stellae classium C—S (atque R, N, T, L) sunt "stellae peculiares," hoc est stellae quae spectrum "peculiare" habent.
 
|style="background:#f8f7ff;"| albus
| 1.7 [[Massa solaris |M<sub>&#9737;</sub>]]
| 1.3 [[RaрадиусRadius solaris|R<sub>&#9737;</sub>]]
| 6 [[Luminocitas solaris|L<sub>&#9737;</sub>]]
| medii
| 3%
|- style="background:#fff4ea;"
!style="background:#fff4ea;"| [[#ClassisGClassis G|G]]
| 5,000–6,000 K
|style="background:#fff2a1;"| flavus
| 8%
|- style="background:#ffd2a1;"
!style="background:#ffd2a1;"| [[#КлассClassis K|K]]
| 3,500–5,000 K
|style="background:#ffc46f;"| aurantinus
| 13%
|- style="background:#ffcc6f;"
!style="background:#ffcc6f;"| [[#lassisClassis M|M]]
| 2,000–3,500 K
|style="background:#ff6060;"| Ruber
 
== Classificatio Yerkes ==
Factor supplementaruis afficiens in characterem spectri est densitas stratorum exteriorum stellae, dependens a massa et densitate stellae, hoc est a luminositate. Admodum a lumnositate [[stroncium|Sr]]IISrII, [[Barium|Ba]]II, [[Ferrum|Fe]]II, [[Titanium|Ti]]II dependunt, propterea est differentia spectrorum stellarum gigantum et pumilionum aequalibus classibus Harvardianis.
 
Ha clssificatione stella habet classem luminocitatis:
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