Info iconThis preview shows page 1. Sign up to view the full content.

View Full Document Right Arrow Icon
This is the end of the preview. Sign up to access the rest of the document.

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 d...
View Full Document

This document was uploaded on 03/04/2014 for the course ASTROPHYS 362 at Minnesota State University Moorhead .

Ask a homework question - tutors are online