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What is the balmer spectrum?
The Balmer series is a set of spectral lines in the visible region of the electromagnetic spectrum of hydrogen. It consists of four lines in the visible light spectrum resulting from transitions in hydrogen's electron shell to the second energy level. The Balmer series is significant in understanding atomic structure and spectroscopy.
What are the wavelengths of the first lines in the Balmer series?
The first lines in the Balmer series of hydrogen correspond to transitions to the n=2 energy level. The wavelengths of these lines are 656.3 nm (Hα), 486.1 nm (Hβ), 434.0 nm (Hγ), and 410.2 nm (Hδ).
What is the maximum wavelength of balmer series?
The Balmer series is a series of spectral lines in the hydrogen spectrum that corresponds to transitions from energy levels n > 2 to the n=2 level. The longest wavelength in the Balmer series corresponds to the transition from n = ∞ to n = 2, known as the Balmer limit, which is approximately 656.3 nm.
What are the wavelengths of the lines in the hydrogen emission spectrum?
The four spectral lines of the Balmer series that fall in the visible range are: 656.3 nm . . . . red 486.1 nm . . . . cyan 434.1 nm . . . . blue 410.2 nm . . . . violet There are four more lines in the Balmer series ... all in the ultraviolet ... and at least thirty-six observable lines altogether from the hydrogen atom.
Why the distances between the lines for the hydrogen spectrum decreases with the decrease in wavelength?
The distances between lines in the hydrogen spectrum decrease with decreasing wavelength because the energy levels in hydrogen are quantized, meaning they can only exist at certain discrete values. As the wavelength decreases, the energy difference between adjacent levels also decreases, resulting in lines being closer together in the spectrum.
Why do the Balmer lines of hydrogen exhibit a phenomenon where they get closer together as you move towards shorter wavelengths?
The Balmer lines of hydrogen exhibit a phenomenon where they get closer together as you move towards shorter wavelengths because of the energy levels of the hydrogen atom. As the electron transitions from higher to lower energy levels, the wavelengths of light emitted become shorter, causing the lines to converge.
What is the balmer spectrum?
The Balmer series is a set of spectral lines in the visible region of the electromagnetic spectrum of hydrogen. It consists of four lines in the visible light spectrum resulting from transitions in hydrogen's electron shell to the second energy level. The Balmer series is significant in understanding atomic structure and spectroscopy.
Why are the hydrogen Balmer lines strong in the spectra of medium temperature stars and weak in the spectra of hot and cool stars?
Balmer lines are produced by colliding hydrogen atoms with electrons excited to 2nd energy level. Cool stars don't have enough collision to excite the electrons, hot stars have too much collision and excite the electrons beyond 2nd energy level.
Why don't they see hydrogen Balmer lines in the spectra of stars with temperatures of 3200 K?
These stars are so cool that nearly all of the hydrogen atoms are in the ground state. The visible-light Balmer absorption lines of hydrogen are produced by electrons moving from the 1st excited state to a higher orbit. However in M class stars most of the hydrogen is in the ground state, and absorption from the the ground state occurs at ultraviolet wavelengths.
What has the author Percy Lowe written?
Percy Lowe has written: 'Structure of the Balmer series lines in the spectrum of hydrogen'
What are the absorption lines in the infrared portion of the spectrum of a star that are produced by hyrdrogen are from?
The absorption lines in the infrared portion of the spectrum of a star produced by hydrogen are primarily the Paschen series. These lines are transitions of electrons in hydrogen atoms from higher energy levels to the third energy level (n=3). Typical Paschen series lines in the infrared include Paschen-alpha at 1.875 μm and Paschen-beta at 1.282 μm.
What are the wavelengths of the first lines in the Balmer series?
The first lines in the Balmer series of hydrogen correspond to transitions to the n=2 energy level. The wavelengths of these lines are 656.3 nm (Hα), 486.1 nm (Hβ), 434.0 nm (Hγ), and 410.2 nm (Hδ).
What is the maximum wavelength of balmer series?
The Balmer series is a series of spectral lines in the hydrogen spectrum that corresponds to transitions from energy levels n > 2 to the n=2 level. The longest wavelength in the Balmer series corresponds to the transition from n = ∞ to n = 2, known as the Balmer limit, which is approximately 656.3 nm.
Contour lines that are closer together indicate a steeper what?
Contour lines that are closer together indicate a steeper slope. The closer the lines are together, the greater the slope of the terrain.
Why are the hydrogen Balmer lines strong in the spectra of medium-temperature stars and weak in the spectra of hot and cool stars?
They are like this due to the fact that most hydrogen atoms are ionized which makes a weaker balmer line. The strength of the Balmer line is sensitive to temperature so that's why it occurs more in the middle. The hot end of the hydrogen is low Balmer line due to them being in the ground state. Hope that's answers it =] -CRS
Is Balmer series only present in hydrogen atom?
No, the Balmer series is observed in hydrogen-like atoms, which have one electron orbiting a nucleus. It consists of the spectral lines produced when the electron transitions from higher energy levels to the second energy level. Other atoms with similar electron configurations can also exhibit Balmer-like series in their spectra.
What are the colours in the balmer series?
The Balmer series consists of visible spectral lines emitted by hydrogen atoms when electrons transition from higher to lower energy levels. The colors in the Balmer series include red (656.3 nm), blue-green (486.1 nm), and violet (434.0 nm) wavelengths.
