Our sun, currently a yellow dwarf, will eventually evolve to a red giant star and then to a white dwarf star as shown in the figure. Assume that the sun radiates like a blackbody. Calculate the power radiated by the YELLOW DWARF sun if its surface temperature is 5778 K.
Our sun, currently a yellow dwarf, will eventually evolve to a red giant star and then to a white dwarf star as shown in the figure. Assume that the sun radiates like a blackbody. Calculate the power radiated by the YELLOW DWARF sun if its surface temperature is 5778 K.
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Our sun, currently a yellow dwarf, will eventually evolve to a red giant star and then to a white dwarf star as shown in the figure. Assume that the sun radiates like a blackbody. Calculate the power radiated by the YELLOW DWARF sun if its surface temperature is 5778 K.
Transcribed Image Text:Stefan-Boltzmann Law:
P(T) = σAT4
Sun
Yellow Dwarf
RYD
O 4.40 x 10^(16) W
O 8.93 x 10^(34) W
O 3.85 x 10^(26) W
O 3.06 x 10^(25) W
=
6.96 × 108 m
RRG
=
o = 5.670×10-8 W/(m² · K4)
White Dwarf
RWD = 6 × 106 m
Red Giant
6.96 × 10¹0 m
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