The spectrum of sunlight contains a set of dark lines named after the German physicist Joseph von Fraunhofer who observed them in 1814. The lines are caused by absorption of light at specific wavelengths by chemical elements present in the solar and terrestrial atmospheres. Features in the photosphere, normally lost in the glare of sunlight, become visible when the Sun is viewed through a narrow band filter tuned to the wavelength of a Fraunhofer line.
This slideshow shows the appearance of the Sun at these wavelengths and the chemical element(s) responsible. All images were processed identically with no enhancement in order to preserve the natural limb darkening of the Sun. The image on the left depicts the true colour. The grayscale image aids in perceiving detail in the violet, blue and red parts of the spectrum.
Best viewed at 4K resolution.
The images were captured with a homemade spectroheliograph:
80 mm aperture f 22.5 telescope
25 µm optical slit
900 mm focal length spectroscope
2400 lines / mm diffraction grating
Toshiba Semiconductor TCD1501D image sensor
Негізгі бет The appearance of the Sun at Fraunhofer line wavelengths: 2 June 2024 (7 lines of hydrogen included)
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