Chapter 11 Bradt Notes ASTR 402 Dr. H. Geller

Slides:



Advertisements
Similar presentations
Astronomy Notes to Accompany the Text Astronomy Today, Chaisson, McMillan Jim Mims.
Advertisements

Universe Eighth Edition Universe Roger A. Freedman William J. Kaufmann III CHAPTER 5 The Nature of Light CHAPTER 5 The Nature of Light.
Stimulated emissionSpontaneous emission Light Amplification by Stimulated Emission of Radiation.
NASSP Masters 5003F - Computational Astronomy Lecture 10 Today I plan to cover: –A bit more about noise temperatures; –Polarized radio signals;
Wavelength, Frequency, and Energy Practice Problems
ASTR Spring 2008 Joel E. Tohline, Alumni Professor 247 Nicholson Hall [Slides from Lecture20]
Atomic Absorption Spectroscopy (AAS) The Visible Spectra.
Black body radiation and ultraviolet catastrophe
Sub-THz Component of Large Solar Flares Emily Ulanski December 9, 2008 Plasma Physics and Magnetohydrodynamics.
Astrophysical Radiative Processes Shih-Ping Lai. Class Schedule.
Spectrum from a Prism. Example of a Spectrum Kirchoff’s Laws.
Spectroscopy 1: Rotational and Vibrational Spectra CHAPTER 13.
Light. What is Light? The third form of energy The only thing astronomers study Electromagnetic radiation The thing that our eyes detect How radio works.
Physics 681: Solar Physics and Instrumentation – Lecture 4
Photons of Light The smallest unit of light is a photon A photon is often called a particle of light The Energy of an individual photon depends on its.
ASTR 2310: Chapter 5 Interaction of Radiation and Matter Atomic Structure Atomic Processes Emission and Absorption Spectra Equation of Radiation Transfer.
Electromagnetic Waves
Lecture 5 An Introduction to Spectroscopy Electromagnetic radiation, electromagnetic wave Emission, absorption, fluorescence.
Thermo & Stat Mech - Spring 2006 Class 21 1 Thermodynamics and Statistical Mechanics Blackbody Radiation.
Lecture 13: Searching for planets orbiting other stars I: Properties of Light 1.How could we study distant habitats remotely ? 2.The nature of light -
LECTURE 6, SEPTEMBER 9, 2010 ASTR 101, SECTION 3 INSTRUCTOR, JACK BRANDT 1ASTR 101-3, FALL 2010.
Chapter 38.
Quantum physics. Quantum physics grew out failures of classical physics which found some quantum remedies in the Planck hypothesis and wave-particle duality.
Solar Spectrum. Bit of Administration …. c = 3 x 10 8 m/sec = 3 x 10 5 km/secc = 3 x 10 8 m/sec = 3 x 10 5 km/sec Reading Reading –BSNV pp
Spectroscopy and Atomic Structure.
Chapter 4 Spectroscopy Chapter 4 opener. Spectroscopy is a powerful observational technique enabling scientists to infer the nature of matter by the way.
Chapter 18 Bose-Einstein Gases Blackbody Radiation 1.The energy loss of a hot body is attributable to the emission of electromagnetic waves from.
Electromagnetic Radiation. Is light a wave or a particle? Yes It’s both, and neither At atomic scales, we have no exact analogs for phenomena For some.
Stars and Galaxies 28.1 A Closer Look at Light Chapter 28.
Lecture II Light spectra. The Birth of the Quantum Max Planck –The energy contained in radiation is related to the frequency of the radiation by the relationship.
PHY418 PARTICLE ASTROPHYSICS Radio Emission 1. Radio emission and particle astrophysics 2 Why are the.
Photon Statistics Blackbody Radiation 1.The energy loss of a hot body is attributable to the emission of electromagnetic waves from the body. 2.The.
Chapters: 3and 4. THREE MAIN LIGHT MATTER INTERRACTION Absorption: converts radiative energy into internal energy Emission: converts internal energy into.
Slide # 1 Variation of PL with temperature and doping With increase in temperature: –Lattice spacing increases so bandgap reduces, peak shift to higher.
Atom and Light ASTR 14: Exploring the Universe. 2 Outline Nature of Light Basic Properties of Light Atomic Structure Periodic Table of the Elements Three.
What is light? Light can act either like a wave or like a particle Particles of light are called photons.
Atomic transitions and electromagnetic waves
What is a Spectrum? How much of observed light is high energy radiation and how much is low energy radiation.
Elemental Analysis using Atomic Absorption and Emission Spectroscopy Bodhisatwa Das.
Chapter 4 Spectroscopy The beautiful visible spectrum of the star Procyon is shown here from red to blue, interrupted by hundreds of dark lines caused.
Chapter 4.
Universe Tenth Edition Chapter 5 The Nature of Light Roger Freedman Robert Geller William Kaufmann III.
Basic Definitions Specific intensity/mean intensity Flux
Blackbody Radiation A blackbody is something that absorbs all radiation that shines on it Are all blackbodies black? - no!! - imagine a box full of lava.
Chapter 9 Bradt’s Astronomy Methods Outline of Chapter Concepts ASTR 402 Observational Astronomy Dr. H. Geller Department of Physics and Astronomy George.
Blackbody. Kirchhoff’s Radiation  Radiated electromagnetic energy is the source of radiated thermal energy. Depends on wavelengthDepends on wavelength.
High Energy Observational Astrophysics. 1 Processes that emit X-rays and Gamma rays.
MOLECULAR SPECTROSCOPY
The Study of Light. The Electromagnetic Spectrum  includes gamma rays, X-rays, ultraviolet light, visible light, infrared radiation, microwaves, and.
Heat Transfer RADIATION HEAT TRANSFER FUNDAMENTALS.
The Study of Light.
The Mechanisms of Electromagnetic Emissions
© 2017 Pearson Education, Inc.
Studying the Sun Notes H- Study of Light Chapter 24
Newton studies the Sun’s spectrum
Really Basic Optics Instrument Sample Sample Prep Instrument Out put
Why Light, why now?.
Radiative Field (Hubeny & Mihalas Chapter 3)
Joel E. Tohline, Alumni Professor
Solar Spectrum wavelength in Å Joseph von Fraunhofer, 1814.
Chapter 4.
(EMR) Electromagnetic Radiation
Electromagnetic Radiation
Radiation in the Atmosphere
Sections 6.1 – 6.3 Electromagnetic Radiation and its Interaction with Atoms Bill Vining SUNY College at Oneonta.
Continuous, Emission, and Absorption
Atomic transitions and electromagnetic waves
Doppler Effect The Doppler Effect is the motion induced change in the observed frequency of a wave. The effect can only be observed/seen due to the relative.
Electromagnetic Radiation
5.4 Learning from Light Our goals for learning
Presentation transcript:

Chapter 11 Bradt Notes ASTR 402 Dr. H. Geller Spectroscopy Chapter 11 Bradt Notes ASTR 402 Dr. H. Geller

Plots of Spectra Emission Line Broadened Emission Line

Plots of Spectra Absorption Lines Continuous Spectra

Plots of Spectra Jargon Energy specific intensity Number specific intensity Photon energy Energy spectral flux density Number spectral flux density Spectral reference band Frequencies and wavelengths Spectral bin widths

Transitions Bound-bound Free-bound Bound-free Free-free

Thermal Bremsstrahlung

Plasmas

Shock Wave

Synchrotron Radiation

Planck Radiation Law Different View from Textbook

Rayleigh Jeans Law

Cosmic Microwave Background

Stellar Spectra

Fraunhoffer Spectrum

Equivalent Width

FWHM

Feedback: Privacy Policy Feedback
Do Not Sell My Personal Information
About project: SlidePlayer Terms of Service

© 2025 SlidePlayer.com. Inc. All rights reserved.