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.
I believe they are primarily within the frequencies of red. I believe it's called the 'Alpha Hydrogen' spectrum or something like that.
Four lines: an UV-band, dark blue, light blue and red band.
Four lines. H alpha, H beta, H gamma and H delta are those four lines visible seen in Balmer series.
Shut up fool
ultraviolet
1
A range of wavelenghs of frequencies of electromagnetic raditation
The series of lines in an emission spectrum caused by electrons falling from energy level 2 or higher (n=2 or more) back down to energy level 1 (n=1) is called the Lyman series. These emission lines are in the ultra-violet region of the spectrum.
wavelengths of absorbed or emitted photons
Just one line for hydrogen.
The emission spectrum of a star is the spectrum of frequencies for emitted electromagnetic radiation during the transition of an atom's electrons from a high-energy state to a low-energy state. The emission spectrum can differ depending on the temperature and composition of the star.
Emission spectrum: lines emitted from an atom.Absorption spectrum: absorbed wavelengths of a molecule.
It differs by that white light spectrum is continuous and consists of light of all wavelengths. Emission spectrum is not continuous. It consists of bright lines at specific wavelengths, with complete darkness between them.
it is a set of lines corresponding to photon emission wavelengths.
Niels Bohr studied the emission lines of Hydrogen.
Rydberg
A range of wavelenghs of frequencies of electromagnetic raditation
Barium produces emission lines at at least 21 different wavelengths in the visible range, including at least one each in red, orange, yellow, green, blue, indigo, violet.
Emission spectra are bright-line spectra, absorption spectra are dark-line spectra. That is: an emission spectrum is a series of bright lines on a dark background. An absorption spectrum is a series of dark lines on a normal spectrum (rainbow) background.
'Astronomical spectrum' is not a specific term. I suspect you are thinking of the emission spectrum of a star, which can tell us a great deal about the composition of the star. Light and other radiations from the object are spread out into constituent wavelengths and dark lines appear across the spectrum at certain specific wavelengths which are characteristic of elements present.
Niels Bohr had the first theoretical explanation. It was based on his very early quantum mechanics - that has now been completely scrapped.
transition of an electron from a higher energy level to a lower energy level.
The spectrum that she will be observing is called an emission spectrum, in which electrons are excited to a higher energy state and then drop back down to the ground state, during which the electrons will emit photons of specific wavelengths, which will be observed as bright lines of color on what appears to be a black background.