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Unformatted text preview: ation describing the emission of blackbody radiation, Eq. (3.16).
Calculate the energy per second absorbed by the average person,
expressed in watts.
d. Calculate the net energy per second lost by the average person via
blackbody radiation.
5. [C&O 3.9] Consider a model of the star Dschubba (δ Sco), the center star in the
head of the constellation Scorpios. Assume that Dschubba is a spherical
blackbody with a surface temperature of 28,000K and a radius of 5.16×109 m. Let
this model star be located at a distance of 123 pc from Earth. Determine the
following for the star:
a. Luminosity (both in Watts and L ).
b. Absolute bolometric magnitude (NOTE: the Sun’s absolute bolometric
magnitude was found to be +4.74 in example 3.2.2).
c. Distance modulus.
d. Apparent bolometric magnitude.
e. Radiant flux at the star's surface.
f. Radiant flux at Earth's surface (compare this with the solar irradiance at
the Earth of roughly 1360 W/m2).
g. Peak wavelength λmax. – Page 2 of 3 – [Problems 6 and 7 are relatively easy as long as you determine what happens to the
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This document was uploaded on 03/04/2014 for the course ASTROPHYS 362 at Minnesota State University Moorhead .
 Spring '14
 Dr.JuanCabanela

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