When the wavelength decreases, that's known as a "blue shift", because
the color of any visible light shifts toward the blue end of the spectrum.
That phenomenon is associated with a light source that's moving TOWARD
the observer.
To find the wavelength of a spectral line using a diffraction grating, you can use the formula: dsin(θ) = mλ, where d is the spacing of the grating lines, θ is the angle of diffraction, m is the order of the spectral line, and λ is the wavelength of the light. By measuring the angle of diffraction of the spectral line and knowing the grating spacing, you can calculate the wavelength of the light.
Green.
The spectral lines from distant galaxies do not match those on Earth because of the Doppler effect, cosmic expansion, and differences in elements present in the galaxies. These factors cause the observed spectral lines to be shifted or altered compared to what we see on Earth.
the intensity of radiation emitted at that wavelength, giving a characteristic spectral distribution that depends only on the temperature of the object emitting the light.
Use the Rydberg formula. A useful article about this is on Wikipedia. It is called "Hydrogen spectral series".
The relationship between the wavelength of a spectral line and its energy is inverse. This means that as the wavelength decreases, the energy of the spectral line increases, and vice versa.
When the wavelength of spectral light emitted from an object increases, it moves towards the red end of the visible light spectrum, also known as the redshift. This indicates that the object is moving away from Earth.
Germanium has a maximum spectral response at around 1.8 µm wavelength, while silicon's maximum spectral response is at around 1.1 µm wavelength.
If the wavelength decreases, the spectral line moves towards the blue end of the visible light spectrum. This phenomenon is known as blue shift, indicating that the object is moving towards Earth.
To find the wavelength of a spectral line using a diffraction grating, you can use the formula: dsin(θ) = mλ, where d is the spacing of the grating lines, θ is the angle of diffraction, m is the order of the spectral line, and λ is the wavelength of the light. By measuring the angle of diffraction of the spectral line and knowing the grating spacing, you can calculate the wavelength of the light.
When the wavelength of spectral lines emitted from an object decreases, it moves towards the violet end of the visible light spectrum. This is known as a blueshift, indicating that the object emitting the light is moving towards Earth.
Green.
As the frequencies of pure spectral colors increase, the wavelengths of the colors will decrease. This is because frequency and wavelength are inversely proportional in electromagnetic waves, according to the equation λν = c, where λ is the wavelength, ν is the frequency, and c is the speed of light.
The wavelength of yellow sodium light in water is approximately 589 nanometers. This specific wavelength is characteristic of the spectral emission line of sodium when it is viewed through water.
A spectral line
The shortest wavelength present in the Brackett series of spectral lines is in the infrared region around 1.46 micrometers. This series represents transitions in hydrogen atoms from higher energy levels to the n=4 energy level.
Barium has an atomic spectra of lines, not only one line (with one wavelength); I reccomend to consult a catalog of spectral lines. See the link below.