Lecture 21 Quantum Physics I. Chapter 27.1 27.5. Outline. Blackbody Radiation The Photoelectric Effect X-Rays The Compton Effect. Blackbody Radiation. Objects at any temperature emit EM radiation that is often referred to as thermal radiation .

ByEP3. Determining the Equilibrium or Planck temperature of a Planet in the absence of an atmosphere. Energy Balance. T s. Shortwave (visible) radiation emitted by sun heats up surface of the Earth. Earth then radiates IR radiation as a blackbody

By0. The Trigonometric Parallax. B. d. p. d = (1/p[arcsec]) parsec. B = 1 AU = 1.496*10 13 cm. 1 pc = 3.26 LY ≈ 3*10 18 cm. 0. The Moving Cluster Method. v. q. v f. v r. q. f. x. 0.

ByStars. Introduction To “Atomic Astrophysics and Spectroscopy” (AAS) Anil Pradhan and Sultana Nahar Cambridge University Press 2011 Details at: www.astronomy.ohio-state.edu/~pradhan/Book/book.html. The Sun – X-Ray Image (YOHKOH Satellite).

ByLight . Lecture 9. By reading this chapter, you will learn. 5-1 How we measure the speed of light 5-2 How we know that light is an electromagnetic wave 5-3 How an object’s temperature is related to the radiation it emits

ByDES Sky Camera (Cloud Camera). Douglas L. Tucker (FNAL) Cloud Camera Review 3 January 2008. SkyCam Purpose. An All-Sky Camera is needed in order to:. Provide real-time estimates of the sky conditions for survey strategy

ByChapter 5: Light. Measuring the speed of light. Early attempts to measure the speed of light were done in 1638 by an apprentice of Galileo

ByBlackbody Radiation. Astrophysics Lesson 9. Homework. None today, module exams?. Learning Objectives. Define the term blackbody. Sketch and describe how shape of black body curves change as temperature is increased.

By20 th century cosmology. 1920s – 1990s (from Friedmann to Freedman) theoretical technology available, but no data 20 th century: birth of observational cosmology Hubble’s law ~1930 Development of astrophysics 1940s – 1950s Discovery of the CMB 1965 Inflation 1981

ByBasic Properties of Stars - 4 §3.4-3.6. Colours of stars and blackbody radiation. Colours of stars. Stars have colours. Why?. Colours of stars. Stars have colours. Why? Its not due to their redshift!!. Betelgeuse: red. Rigel: blue-white. Blackbody Radiation. Surface Temp = 3600K.

BySolar Energy. On how the Sun emits energy as radiation, and how the Earth receives it. Outline. Blackbody radiation and the Sun. Wien’s law Stefan-Boltzmann law The temperature and spectrum from the Sun. The Earth as receiver The Solar Constant The wobbly Earth

By3 - Light. The Wave Nature of Light. Wavelength λ - Units: meters (m), μ m , nm Frequency ν or f - Unit: cycles/s, universally called Hertz (1 Hertz = 1 cycle/s)

ByWeek 5 – September 30, 2003. Blackbody radiation: Monochromatic irradiance of radiation emitted by a blackbody at (absolute) temperature T is given by: = When C 2 = 3.74 x 10 -16 Wm 2 C 2 = 1.44 x 10 -2 m o k Blackbody radiation is isotopic Eλ C 1 λ -5 e (-C2/λT) λm =.

ByBlackbody Radiation. Blackbody: an object that absorbs and emits all radiations of all possible frequencies

ByWeek 5 – September 30, 2003. Blackbody radiation: Monochromatic irradiance of radiation emitted by a blackbody at (absolute) temperature T is given by: = When C 2 = 3.74 x 10 -16 Wm 2 C 2 = 1.44 x 10 -2 m o k Blackbody radiation is isotopic Eλ C 1 λ -5 e (-C2/λT) λm =.

ByBlackbody Radiation. Blackbody: an object that absorbs and emits all radiations of all possible frequencies

ByFractional Blackbody Emissive Power Solver. By: David Wheeler & William Tryon November 30, 2011. Introduction. It is often necessary to know the fraction of the total emission from a blackbody that is in a certain wavelength interval or band.

ByBlackbody Radiation. A blackbody is something that absorbs all radiation that shines on it Are all blackbodies black? no!! imagine a box full of lava. A constant temperature blackbody (a.k.a. a very precise oven). Order your own blackbody online. Blackbodies and Astronomy.

ByLecture #8: Blackbody Radiation, Einstein Coefficients, and Homogeneous Broadening. Substitute Lecturer: Jason Readle Thurs, Sept 17 th , 2009. Topic #1: Blackbody Radiation. What is a Blackbody?. Ideal blackbody: Perfect absorber Appears black when cold!

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