What kind of spectrum does the photosphere produce?
What kind of spectrum does the photosphere produce?
Absorption Spectrum
The Sun’s Spectrum is an Absorption Spectrum Only at the wavelengths at which atoms in the photosphere can absorb light will photons be impeded in their outward travel. The result is an absorption spectrum, a continuous blackbody spectrum with dark absorption lines superimposed on it.
Does the photosphere emit radiation?
The visible photosphere, or sphere of light, is the level of the solar atmosphere from which we get our light and heat, and it is the part that we can see with our eyes. Also, the photosphere is too cool to emit intense radiation at these wavelengths, so it appears dark under the hot gas.
Why the photosphere shows an absorption spectrum while the chromosphere shows an emission spectrum?
However, the photosphere is made of plasma and gas that is about 5800 K, so the gas will absorb some of the energy as the photons pass outwards through the photosphere. This creates absorption lines in the solar spectrum. Similarly, the chromosphere is heated to temperatures around 25,000 K.
What are the wavelengths of mercury?
The wavelengths of the prominent lines in mercury are purple (405 nm), blue (436 nm), blue- green (492 nm), greenish yellow (546 nm), yellow (577 nm), orange (623 nm), and red (691 nm). Remember that 1 nm = 10-9 m.
Why we can see into the photosphere but no deeper into the Sun?
Since the Sun is made up of hot gas, there isn’t really a “surface” to it. Instead, as you move from space toward the Sun’s core, the gas gets denser and denser. The photosphere represents the depth at which we can see no deeper toward the core of the Sun.
Is the corona hotter than the photosphere?
Edlén and Grotrian’s finding that the sun’s corona is so much hotter than the photosphere – despite being further from the sun’s core, its ultimate source of energy – has led to much head-scratching in the scientific community.
Why is the photosphere important?
The lowest layer of the sun’s atmosphere is the photosphere. It is about 300 miles (500 kilometers) thick. This layer is where the sun’s energy is released as light. Because of the distance from the sun to Earth, light reaches our planet in about eight minutes.
What is mercury spectrum?
There is a substantial number of standard spectral lines of mercury, which can be produced with mercury-based spectral lamps; typical wavelengths are 184.5 nm, 253.7 nm, 365.4 nm, 404.7 nm, 435.8 nm, 546.1 nm, 578.2 nm and 1014 nm.
What color is mercury when excited?
Color
| Gas | Color | Notes |
|---|---|---|
| Used in carbon dioxide lasers. | ||
| Mercury vapor | Light blue, intense ultraviolet | In combination with phosphors used to generate many colors of light. Widely used in mercury-vapor lamps. |
| Sodium vapor (low pressure) | Bright orange-yellow | Widely used in sodium-vapor lamps. |
Can we see inside the Sun?
We can’t see inside the Sun in ordinary visible light directly, because gas in the photosphere is so dense that it absorbs and scatters all photons coming from below. However, we can use visible light to probe the solar interior indirectly, by looking at very subtle pulsations of the photosphere.
What are the emission lines in a mercury vapor lamp?
Only the light at 253 nm is usable unless synthetic quartz is used to manufacture the tube as the line is otherwise absorbed. In medium-pressure mercury-vapor lamps, the lines from 200–600 nm are present.
How are the emission spectra of hydrogen and helium related?
Notice the differences in the emission spectra for hydrogen (H), helium (He) and mercury (Hg), that are shown in Fig. 10.4. The energy of an emitted photon and its wavelength are related. For example, the color of a laser pointer (e.g. red or green) is determined by the energy of the emitted light.
Why are only certain wavelengths of light allowed in emission spectra?
Therefore, when you are measuring the emission spectrum of an element, only certain wavelengths of light are allowed and the “pattern” that is produced is unique for that substance. Notice the differences in the emission spectra for hydrogen (H), helium (He) and mercury (Hg), that are shown in Fig. 10.4.
What are the colors of the light spectrum?
Standard Spectral Lines Wavelength Color Designation Element 365.0146 nm ultraviolet i mercury 404.6561 nm violet h mercury 435.8343 nm blue g mercury 479.9914 nm blue F’ cadmium