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Starlight: how the physics of electromagnetism provides a key to the stars

Discover how the physics of light and electromagnetism provide key insights into the stars and their properties. Learn about the spectrum of light and its different wavelengths, and how spectroscopy helps extract valuable information from starlight. Explore Kirchoff's laws, Wien's law, and their application in studying star spectra. See examples of stellar spectra and understand how they reveal temperature, composition, and other properties. Uncover the fascinating world of starlight through the application of spectroscopy.

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Starlight: how the physics of electromagnetism provides a key to the stars

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  1. Starlight: how the physics of electromagnetism provides a key to the stars

  2. Light is the only information we get from most astronomical objects. To understand these objects, we need to understand the physics of light and how it is produced.

  3. First result: light is a wave (electromagnetic wave) Wave characterized by wavelength, amplitude DEMO

  4. Amazing fact of nature: wide range of wavelengths of electromagnetic waves EM radiation includes gamma rays, x-rays, ultraviolet, Light, infrared, microwave, radio

  5. Concept from physics crucial for astronomy: the spectrum of light Will do in lab this week (or soon); DEMO

  6. Spectra (plural of spectrum) • A fundamental measurement to extract more information from starlight • Spread out light according to wavelength • See Section 16.5 The solar spectrum

  7. The Solar Spectrum as an astronomer would study it

  8. What do the spectra of the Sun and stars tell us about those objects? See Figure 16.11 from book http://www.astro.umd.edu/~ssm/ASRT220/OBAFGKM.html

  9. The Physics of Spectrum Formation, Kirchoff’s Laws and Wien’s Law • Hot opaque solid or liquid produces a continuous spectrum • Hot, tenuous gas observed against dark background produces emission line spectrum • Cold, tenuous gas observed against bright background produces absorption spectrum • See Figure 16.6

  10. Kirchoff’s Laws of Radiation

  11. Kirchoff’s First Law + Wien’s Law • Hot, opaque objects produce continuous spectrum • The hotter the object, the bluer it is • Wien’s Law wmax = 2.9E-03/T • The hotter an object, the brighter it is • demo

  12. Why does Wien’s Law look like that? A physicist is bothered when he or she sees an equation like: The form which emerges from fundamental equations of physics is:

  13. Kirchoff’s First Law + Wien’s Law

  14. Kirchoff’s 2nd Law: Emission Line Spectra Wavelengths of emission lines unique “fingerprint” of element

  15. Kirchoff’s Third Law: Absorption Spectra See Figure 16.6

  16. Starlight…application of spectroscopy to stars • Continuous spectrum gives surface temperature (Wien’s Law) • Spectral lines give chemical composition, temperature (also), speed of rotation (How?) and other properties • Examples of stellar spectra…what can we say?

  17. Spectral classes of stars: O,B,A,F,G,K,M What can you say about the temperatures of these stars?

  18. Examples of stellar spectra Question: apply Wien’s Law to the O5 star. What Can you say about its Temperature (relative to the Sun?)

  19. With information provided by spectroscopy, we can search for correlations between stellar properties

  20. What the data show: the Hertzsprung-Russell Diagram Highest quality data from the Hipparchus spacecraft

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