The wavelength of maximum solar emission is observed to be approximately 0.475 μm. What is the surface temperature of the sun (assumed as blackbody)?
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- The sun can be modeled as a blackbody emitting at a temperature of 5800.0 Kelvin. Determine the following: a) The blackbody emissive power of the sun. b) The fraction of the sun’s emission in the visible range (0.40μm – 0.70μm).What is the vrms of hydrogen on the surface of the sun if its temperature is 5.36E3 degC? What is the vrms of hydrogen on the surface of the earth if its temperature is 21.2 degC?A window has heavy curtains in front of it. At night the curtains are closed to minimise heat loss. During the day the curtains are pulled aside exposing the glass window. How much heat is lost through the 1.0 m x 1.0 m square glass window pane that is 4mm thick when the inside temperature is 20 degree C and the outside temperature is -6 C (negative 6.0) in 12 hrs? ( 1m = 100 cm) (1m = 1000mm) %3D
- The next four questions use this description. Our Sun has a peak emission wavelength of about 500 nm and a radius of about 700,000 km. Your dark-adapted eye has a pupil diameter of about 7 mm and can detect light intensity down to about 1.5 x 10-11 W/m2. Assume the emissivity of the Sun is equal to 1. First, given these numbers, what is the surface temperature of the Sun in Kelvin to 3 significant digits? What is the power output of the Sun in moles of watts? (in other words, take the number of watts and divide it by Avogadro's number) Assuming that all of the Sun's power is given off as 500 nm photons*, how many photons are given off by the Sun every second? Report your answer to the nearest power of 10 (e.g. if you got 7 x 1024, give your answer as 25).#19.13 FIND THE GIVEN, REQUIRED, SOLUTION AND EXPLAIN PER STEPSPlease asap
- You have a 5.3 inch diameter sphere heated to 335.0°F, which is inside of a large room with a surrounding temperature of Tsurr = 71.0°F. Treating the sphere as a blackbody, calculate the net heat transfer rate due to radiation between the sphere and its surrounds, in units of BTU/hr. The Stephan-Boltzmann Constant in English units is: σ = 1.714*10-9 BTU/(hr-ft2-°R4).The radiant flux at Earth is 1365 W/m2. Say we move towards the sun to a radius that is 1/3 the radius of the Earth's orbit. By what factor would the radiant flux increase or decrease?