θ r n f (erg cm -2 s -1 hz -1 ) h (erg cm -2 s -1 hz -1 ) f = 4 (r/d) 2 h
TRANSCRIPT
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θ
R
n
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f (erg cm-2 s-1 Hz-1) H (erg cm-2 s-1 Hz-1)
f = 4 (R/D)2 H
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DA starTeff=25,700 K log g=7.98
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Le système des magnitudes
La magnitude apparente «m» (en minuscule)
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La magnitude apparente bolométrique mbol
Bolométrique : flux intégré sur toutes les fréquences
mesure la brillance apparente de l’étoile
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La magnitude absolue bolométrique Mbol
propriété intrinsèque de l’étoile
Le module de distance
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d = p1 avec d en parsec si p est en seconde d’arc
parallaxetrigonométrique ()
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En général on mesure le flux au travers d’une bande passante
Transparence
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Exemple : la magnitude V dans le système photométrique Johnson
Vega :
Module de distance
observé calculé
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Vega
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Indices de couleurs (2 bandes passantes)
Flux d’Eddington
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Température effective
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à = 100, T 30,000 K (Teff / T)4 1% d’anisotropie en I