absorption lines due to the thin outer layer above the photosphere
Light coming up from the centre of the Sun goes through the outer layer where it encounters absorbtion by elements in the outer layer, and this gives rise to absorbtion lines in the spectrum.
There are a lot more. Each element has several possible absorption lines. In fact the element iron has several hundred lines.
The spectrum of a solar prominence reveals information about the elements present in the gas, the temperature, density, and motions of the material within the prominence, as well as magnetic fields influencing its behavior. By studying the spectrum, scientists can gain insights into the physical properties and processes occurring in solar prominences.
The most deviated color in the solar spectrum is blue. This is because the shorter wavelengths of blue light are scattered more easily by the Earth's atmosphere, causing them to appear more spread out compared to longer wavelengths like red.
Visible light has the maximum intensity in the solar electromagnetic spectrum. The Sun emits a range of wavelengths, with visible light falling in the middle of this range. Our eyes are most sensitive to these wavelengths, which is why we perceive sunlight as bright.
Dark lines in the spectrum were named after German physicist Joseph von Fraunhofer, who first systematically studied them. They are commonly known as Fraunhofer lines and are formed when certain chemical elements absorb specific wavelengths of light, creating dark bands in the spectrum.
J. Houtgast has written: 'The variations in the profiles of strong Fraunhofer lines along a radius of the solar disc' -- subject(s): Solar Spectrum, Spectrum analysis, Spectrum, Solar
Fraunhofer lines are observed in the solar spectrum by using a spectroscope to disperse sunlight into its component colors. These dark absorption lines are caused by the absorption of specific wavelengths of light by elements in the Sun's atmosphere. By studying the positions and intensities of these lines, scientists can learn about the composition and physical properties of the Sun.
Fraunhofer lines are dark lines in the solar spectrum caused by absorption of sunlight by elements in the outer layers of the sun. Each element absorbs light at specific wavelengths, creating unique patterns of dark lines. By comparing these patterns to known spectra of elements, scientists can identify which elements are present in a substance.
Joseph von Fraunhofer lived from 1787-1826. He became the director of a scientific institute in Germany. He made some of the best telescope lenses, which he was trained to do. He identified the dark absorption lines that are in the solar spectrum. These lines show scientists which chemical elements are in light.
Joseph Von Fraunhofer as a German physicist who independently discovered (or rediscovered) dark "lines" in the emission spectra of the light emitted by the Sun. Fraunhofer carefully cataloged the precise frequencies of the light that was NOT being emitted by the Sun. Many years later, two other scientists realized that these colors of light were associated with the spectra of particular elements present in the Sun.
· full moon - free fall - far side of the moon - solar faculae - Fraunhofer lines
The dark lines represents the absorption of energy at that frequency, E=hf.
Atomic spectrum is produced when atoms emit or absorb light at specific energies, creating distinct lines or bands. Solar spectrum is the continuous spectrum of light emitted by the Sun, containing all wavelengths of light. Solar spectrum is produced by many elements and compounds in the Sun's atmosphere, creating a broad, continuous range of colors.
Light coming up from the centre of the Sun goes through the outer layer where it encounters absorbtion by elements in the outer layer, and this gives rise to absorbtion lines in the spectrum.
The spectrum of helium consists of distinct lines at specific wavelengths, known as emission lines, due to the transition of electrons between energy levels. In contrast, the spectrum of white light from the Sun is continuous, with all visible wavelengths present. The presence of absorption lines in the solar spectrum, caused by elements in the Sun's atmosphere absorbing specific wavelengths, further distinguishes it from the discrete emission lines of helium.
There are a lot more. Each element has several possible absorption lines. In fact the element iron has several hundred lines.