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Classis spectralis, in astronomia, est divisio stellarum in classes secundum temperaturam vel magnitudinem. Sunt plures classificationes quae inter se differunt.
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 (olim R, N) sunt "stellae peculiares," hoc est stellae quae spectrum "peculiare" habent.
Classis | Temperatura | Color verus | Coror visibilis[1][2] | Massa (in massis Solis) |
Radius (in radiis Solis) |
Luminsoitas | Lineae Hydrogenii | % e stellis seriei capitalis |
---|---|---|---|---|---|---|---|---|
O | 30,000–60,000 K | caeruleus | caeruleus | 60 M☉ | 15 R☉ | 1,400,000 L☉ | debiles | ~0.00003% |
B | 10,000–30,000 K | albus-caeruleus | albus caeruleus albusque | 18 M☉ | 7 R☉ | 20,000 L☉ | medii | 0.13% |
A | 7,500–10,000 K | albus | albus | 3.1 M☉ | 2.1 R☉ | 80 L☉ | lucidi | 0.6% |
F | 6,000–7,500 K | ochroleucus | albus | 1.7 M☉ | 1.3 R☉ | 6 L☉ | medii | 3% |
G | 5,000–6,000 K | flavus | ochroleucus | 1.1 M☉ | 1.1 R☉ | 1.2 L☉ | debiles | 8% |
K | 3,500–5,000 K | aurantius | rutilus | 0.8 M☉ | 0.9 R☉ | 0.4 L☉ | admodum debiles | 13% |
M | 2,000–3,500 K | ruber | flammeus | 0.3 M☉ | 0.4 R☉ | 0.04 L☉ | admodum debiles | >78% |
Factor supplementaruis afficiens in characterem spectri est densitas stratorum exteriorum stellae, dependens a massa et densitate stellae, hoc est a luminositate. Admodum a lumnositate SrII, BaII, FeII, TiII dependunt, propterea est differentia spectrorum stellarum gigantum et pumilionum aequalibus classibus Harvardianis.
Ha clssificatione stella habet classem luminocitatis:
Classificatio Harvardiana definit Abscissam diagrammatis Hertzsprung—Russell, sed Yerkes classificatio — positionem stellae in diagrammate. Supplementaria autem praestantia huius classificationis est possibilitas definendi luminocitatem sellae (spectro cognoto), et propterea possibilitas aestimandi distantionem ad stellam.
Sol, pumilio flava, habet classem spectralem G2V.
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