The infrared radiation coming from the center of our galaxy has a wavelength of 2 µm. Using this wavelength to estimate the temperature of the stars present in the center of the galaxy.
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- Why is SMF faster than MMF over large distances?17.2 (a) Use the fact that fo [2³/(e² − 1)] dz = π¹/15 to show that the total radiant energy emitted per second by unit area of a blackbody is 27³KT4/15c²h³. Note that this quantity is propor- tional to T4 (Stefan's law). (b) The sun's diameter is 1.4 × 10⁹ m and its effective surface temperature is 5800 K. Assume the sun is a blackbody and estimate the rate of energy loss by radiation from the sun. (c) Use E mc² to calculate the relativistic mass of the photons lost by radiation from the sun in 1 year. =Using Wien's Law for two black body objects with a temperature of 1000 K (fire) and 290 K (background), at what central wavelengths are the two objects radiating?
- 4.A certain star's power output is 2.9 x 1026 W. Assuming an ideal radiator with e = 1, calculate its radius in km if its temperature is 5,720 K. The Stefan-Boltzmann constant is 5.67 x 10-8 W/(m².K4). R = > _km 616,612 margin of error +/- 1%3. Consider the following stellar spectra from the sun and from a supercluster of galaxies. ABSORPTION LINES FROM THE SUN ABSORPTION LINES FROMA SUPERCLUSTER OF GALAXIES BAS11 v = 0.07c, d 1 billion light years (a) Describe the movement of the stars in the supercluster relative to the sun. (b) Suppose the absorption lines on the bottom spectrum had varying thickness. What would this indicate about the stars in the supercluster?
- Physics astronomy/dsinė A beam of electrons is shot towards a material X with a crystalline structure. A diffraction pattern is observed corresponding to a distance d=0.15 nm. between two adjacent Bragg planes. The electrons are each sent in with a kinetic energy of 51.900000000000006 eV. Part a) Find the de Broglie wavelength in nanometres of an electron incident on the material X.P X %23 in a 20 poster wal Sp Sp famu.instructure.com/courses/9823/assignments/177283 M Update : THERMAL RADIATION 2 FLORIDA MECHANICAL AGRICULTURA HEAD HEART HAND Problem 4. Planetary Temperatures: Radiation of Heat to Space (Palen, et. al. 1st Ed. Chapter 6 Problem 63 ) FIELD Working It Out 6.2 The Stefan-Boltzmann Law Account Look at Figure 6.17, which shows the spectra of a light source at several different temperatures. This source is assumed to emit electromagnetic radiation only because of its temperature, not its composition. This kind of source is called a blackbody, and if we graph the intensity of its emitted radiation across all wave- lengths (as in Figure 6.17), we obtain a characteristic curve called a blackbody spectrum. As the object's temperature increases, it emits more radiation at every wavelength, so each increase in temperature raises the curve. The luminosity of the object (the total amount of light emitted) increases. In fact, it increases quite fast as the…
- Astronomers use two basis properties of stars to classify them. These two properties are luminosity and surface temperature. Luminosity usually refers to the brightness of the star relative to the brightness of our sun. Astronomers will often use a star’s color to measure its temperature. Stars with low temperatures produce a reddish light while stars with high temperatures shine with a brilliant blue—white light. Surface temperatures of stars range from 3000o C to 50,000o C. When these surface temperatures are plotted against luminosity, the stars fall into groups. Using the data similar to what you will plot in this activity, Danish astronomer Ejnar Hertzsprung and United States astronomer Henry Norris Russell independently arrived at similar results in what is now commonly referred to as the HR Diagram. Procedures:1. Read the Background Information 2. On the graph paper provided. Place a number next to the star according to its luminosity and surface temperature listed in the data…The wavelength of the peak of the blackbody distribution was found to follow Wein’s Displacement Law. Calculate the peak wavelength of a bluish-white star that radiates at temperature 20000 K. a) 145 nm b) 100 nm c) 114 nm d) 155 nmUse Wien's Law to calculate the peak wavelength of light coming from the Sun. Assume T=5800 K for the surface temperature of the Sun. Wein's displacement law says that the blackbody temperature and peak wavelength multiplied together give a constant of 0.29 cm-K. (K is degrees Kelvin). Convert the wavelength from part A into a frequency. The product of wavelength and frequency for electromagnetic radiation is a constant, the speed of light (c), 3 x 10^10 cm/s.