How are stellar EM radiation formed?

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SUMMARY

Stellar electromagnetic (EM) radiation is formed through two primary mechanisms: atomic emission at discrete wavelengths and black body radiation, which produces a continuous spectrum. When a body exceeds 0 K, its atoms vibrate, generating a range of wavelengths due to their random movements. The peak wavelength of emitted radiation shifts with temperature, allowing for temperature determination based on black body radiation principles. Additionally, synchrotron radiation occurs when relativistic electrons spiral in magnetic fields, as seen in astronomical phenomena like the Crab Nebula.

PREREQUISITES
  • Understanding of black body radiation principles
  • Familiarity with atomic emission spectra
  • Knowledge of phonons and photons
  • Basic concepts of synchrotron radiation
NEXT STEPS
  • Study Planck's Law and its application to black body radiation
  • Explore the concept of atomic emission spectra and spectral lines
  • Investigate the relationship between temperature and peak wavelength using Wien's Displacement Law
  • Learn about synchrotron radiation and its implications in astrophysics
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Astronomers, physicists, and students interested in understanding the mechanisms of stellar radiation and its implications in astrophysics.

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How are stellar EM radiation formed??

I've read this in many books and sites... Any object above 0 K will emit EM radiation of all wavelengths... Now this is confusing me a lot... I mean, how for example a sun emit wavelength s of a Radio and it is the same sun which emits ultra violet and gamme rays.. How is it possible to emit all kind of wavelengths. Being particular, when we look at a star by prism method, how can we detect an O star which has it's peak wavelength beyond visible light i guess... Finally, why is a peak wavelength formed. Thanks in advance to whoever gives me a good reply!
 
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This was confusing me too. But I think I found the answer.

Atoms will emit photons at discrete wavelengths - so you can see characteristic lines for gases like hydrogen etc.

Then there is black body radiation - which is a continuous spectra.

And how this happens. When a body is hot, the atoms jiggle against each other, which causes their electro-magnetic fields to interact. This effectively creates lots of phonons - since atoms movements are largely random you get a broad band of wavelengths - a continuous spectra. Some atoms are moving very fast and some are moving very slowly - two fast atoms hit each other head on they'll slow down to a crawl, and then you'll get a radio wave phonon...and the effect is you can get light with really long wavelengths.

The phonons become photons when they leave the body and travel into empty space.

When a body gets hotter - the intensity of the continuous spectra increases - and because the atoms are moving faster, the peak frequency of the spectra gets higher. And you can tell the temperature of a body by knowing the peak frequency of the black body radiation it's emitting.



There's some lovely formulas too, than govern what you see in the spectra...which I can't remember...If anyone else does?
 


Also, spiraling relativistic electrons in magnetic fields near astronomical objects (e.g., Crab nebula) emit a continuous wavelength EM spectrum called synchrotron radiation. See http://en.wikipedia.org/wiki/Crab_Nebula
 

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