Table 1.
Estimated properties of stars of various temperatures.
T⋆ [K] | 20 000 | 35 000 | 50 000 |
---|---|---|---|
Ltotal [L⊙] | 4200 | 2 × 105 | 2 × 106 |
Radius [R⊙] | 5.4 | 11 | 17 |
Mass [M⊙] | 11 | 31 | 60 |
tMS [yr] | 3 × 107 | 2 × 106 | 4 × 105 |
Q⋆ [s−1] | 2.7 × 1046 | 1.9 × 1048 | 3.4 × 1049 |
Nstars | 7.9 × 108 | 7.0 × 107 | 1.5 × 107 |
SFR [M⊙ yr−1] | 300 | 1100 | 2500 |
Notes. L⋆ is the stellar luminosity estimated from the main sequence, followed by the radius required to equate this to the bolometric intensity obtained from the Planck function. The stellar mass is estimated from the mass–luminosity relation, L⋆/L⊙ = (M⋆/M⊙)3.5, and the main sequence lifetime, tMS, from tMS ∝ 1/M2.5. Nstars is the number of stars of this mass according to the Salpeter initial mass function, normalised to a total stellar mass of 3 × 1012 M⊙, followed by the star formation required to maintain this (see main text).
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