Spectral Lines

Jul 02, 2012

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Spectral Lines

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1. Spectral Lines Celestial Fingerprinting

2. Goals From light we learn about Composition Motion

3. Continuum Spectra

Spectral Lines

Spectral Lines. Celestial Fingerprinting. Visit www.worldofteaching.com For 100’s of free powerpoints. Goals. From light we learn about Composition Motion. Emission lines. Absorption lines. Continuum. A Spectrum.

401 views • 22 slides

Spectral Lines

Spectral Lines. Celestial Fingerprinting. Goals. From light we learn about Composition Motion. Emission lines. Absorption lines. Continuum. A Spectrum. A spectrum = the amount of light given off by an object at a range of wavelengths. Temperature and Light. Warm objects emit light.

457 views • 24 slides

The hydrogen lines in spectral type A stars

The hydrogen lines in spectral type A stars. are most narrow for supergiants. are most narrow for main sequence stars. can not be used to estimate the luminosity of the star. are very weak and difficult to see. are useful in determining the apparent magnitude of the star.

2.11k views • 64 slides

Spectral Lines

Spectral Lines. Celestial Fingerprinting. Goals. From light we learn about Composition Motion. The Greenhouse Effect. Why is my car hot on a summer day? At T = 6000 K, the Sun radiates mostly visible light. Windshield is transparent to visible light.

454 views • 28 slides

Spectral Lines

Spectral Lines. Caitlin Campbell . Spectrometer. Instrument used to measure properties of light of the electromagnetic spectrum Enters through optical fiber, spectrometer refracts incoming light splitting into component wavelengths and records intensity with a detector

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Chapter 5 Spectral Lines

Chapter 5 Spectral Lines. Kirchhoff’s Laws describe the p roduction of spectral lines. Continuous spectrum – Hot dense gas or solid objects produces a continuum of wavelengths, with no spectral lines. Emission spectrum – Hot gas produces bright spectral lines.

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Spectral lines analysis

Spring School of Spectroscopic Data Analyses 8-12 April 2013 Astronomical Institute of the University of Wroclaw Wroclaw, Poland. Spectral lines analysis. Rotational velocity and velocity fields. Giovanni Catanzaro INAF - Osservatorio Astrofisico di Catania.

389 views • 23 slides

Spectral Lines

Spectral Lines. Celestial Fingerprinting. Continuum Spectra. The Sun. A Continuum Spectrum: Light emitted across a continuous range of wavelengths. A blackbody spectrum is a continuum spectrum. But what are these?. Heat some gas and it will glow.

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Chapter 13 – Behavior of Spectral Lines

Chapter 13 – Behavior of Spectral Lines. We began with line absorption coefficients which give the shapes of spectral lines. Now we move into the calculation of line strength from a stellar atmosphere. Formalism of radiative transfer in spectral lines Transfer equation for lines

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Spectral Lines

Spectral Lines. Celestial Fingerprinting. http://jersey.uoregon.edu/elements/Elements.html. What we need to know?. How are spectral lines formed? Define the three types of spectra Compare and contrast an absorption and emission spectra What is Kirchhoff law?

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Spectral Lines

327 views • 23 slides

The Formation of Spectral Lines

The Formation of Spectral Lines. Line Absorption Coefficient Line Transfer Equation. Line Absorption Coefficient. Main processes Natural Atomic Absorption Pressure Broadening Thermal Doppler Broadening.

851 views • 67 slides

Spectral Lines

Spectral Lines. Spectral Lines. Gives the frequency composition of the function Amplitude, phase of sinusoidal components Could provide information not found in time signal E.g. Pitch, noise components May help distinguish between signals E.g speech/speaker recognition.

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Polarimetric shapes of spectral lines in solar observations

Polarimetric shapes of spectral lines in solar observations. Egidio Landi Degl’Innocenti Dipartimento di Fisica e Astronomia Università di Firenze, Italia. 9th Serbian Conference on Spectral Line Shapes in Astrophysics. Banja Koviljaca, May 13-17, 2013. Line shapes I.

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Spectral Lines

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11. Spectral Lines II

11. Spectral Lines II. Rutten: 5.1, 5.2 Line formation Eddington-Milne Curve of Growth. Curve of Growth. Curve of Growth is a theoretical plot of line equivalent width against line optical depth, usually plotted as log( W l ) – log( t ).

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Spectral lines

Spectral lines. Photon energy Atomic structure Spectral lines Elements in stars Masses of stars Mass-luminosity relation Reading: sections 16.5, 16.7, 6.2. Photon energy. Up to now, we have been discussing the wavelength of light as determining it color

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Spectral Lines

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10. Spectral Lines I

10. Spectral Lines I. Rutten: 9.1, 3.3 Line strength, equivalent width Line profile Broadening Voigt profile. I l. I l. W l. I c. I l ( l ). l. l. The Line Spectrum. A spectral line is described by its profile. The line depression,

150 views • 12 slides

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