Figure 39.9 The absorption line spectrum of the sun. (The spectrum "lines" read from left to right and from top to bot- tom, like text on a page.) The spectrum is produced by the sun's relatively cool atmosphere, which absorbs photons from deeper, hotter layers. The absorption lines thus indicate what kinds of atoms are present in the solar atmosphere.
Figure 39.9 The absorption line spectrum of the sun. (The spectrum "lines" read from left to right and from top to bot- tom, like text on a page.) The spectrum is produced by the sun's relatively cool atmosphere, which absorbs photons from deeper, hotter layers. The absorption lines thus indicate what kinds of atoms are present in the solar atmosphere.
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To a good approximation, the sun’s surface is a blackbody with a surface temperature of 5800 K. (We are ignoring the absorption produced by the sun’s atmosphere, shown in Fig. 39.9.) (a) At what wavelength does the sun emit most strongly? (b) What is the total radiated power per unit surface area?
Transcribed Image Text:Figure 39.9 The absorption line spectrum
of the sun. (The spectrum "lines" read
from left to right and from top to bot-
tom, like text on a page.) The spectrum
is produced by the sun's relatively cool
atmosphere, which absorbs photons from
deeper, hotter layers. The absorption lines
thus indicate what kinds of atoms are
present in the solar atmosphere.
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