The discussion centers on the emission spectrum of the Sun, clarifying that the continuous spectrum observed is primarily due to thermal motion rather than redshift or blueshift effects. The Sun's radiation follows a blackbody spectrum, with significant contributions from interatomic collisions and thermal energy. Specific hydrogen spectral lines are noted, with the most common photon energy being 1.89 eV. Doppler broadening is acknowledged but deemed insufficient to explain the continuous nature of the spectrum.
PREREQUISITESAstronomers, physicists, and students studying astrophysics or spectroscopy will benefit from this discussion, particularly those interested in the mechanisms behind solar radiation and spectral analysis.
When the temperature of the body is greater than absolute zero, interatomic collisions cause the kinetic energy of the atoms or molecules to change. This results in charge-acceleration and/or dipole oscillation which produces electromagnetic radiation, and the wide spectrum of radiation reflects the wide spectrum of energies and accelerations that occur even at a single temperature.
No. As pointed out above, this is absolutely not the explanation. Doppler broadening of the spectral lines is present, but much too small to produce a continuous spectrum. And the majority of the photons are produced in other ways, simply from the thermal motion of the atoms.edguy99 said:We see all sorts of other photon energies that are generated since the hydrogen on the sun surface is moving around. If the hydrogen atom is moving away from us, we will see a photon with less than 1.89eV (red shifted), if moving towards us, it will have more than 1.89eV energy (blue shifted)
Bill_K said:... much too small to produce a continuous spectrum. And the majority of the photons are produced in other ways, simply from the thermal motion of the atoms.