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These high-temperature stars emit ultraviolet (UV) light that ionizes the surrounding hydrogen atoms into protons (H+) and electrons (e-). When the protons and electrons recombine, the electrons enter a higher energy level (n=3). Then, when the electron drops from the n=3 level to the n=2 level, an H??photon is emitted. 2 This photon has a wavelength of 6563 A, and therefore corresponds to the red portion of the visible spectrum. It is these H? photons which give the nebula the distinctive red color which we see.
The extreme brightness of the O-type and B-type stars, coupled with the Earth's atmosphere, has always made high-resolution imaging of the star-forming region difficult...
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