Wavelengths of absorbed or emitted photons
Every line in a line spectrum is caused by a transition, from one quantum state to another quantum state, involving electrons.
The wave lengths of lines of the spectrum are different for each chemical element.
There are several kinds of spectra. Bright line spectrum, or emission spectrum, is when light emitted by a gas has an electrical discharge going through it, and it produces a spectrum of just a few isolated parallel lines.
Niels Bohr studied the emission lines of Hydrogen.
An absorption spectrum can tell the astronomer or physicist what elements are in the starlight being observed. A diffraction grating is used to split the incoming light into a spectrum of colors. Sodium, for example, causes dark Fraunhofer lines at known points in the visible spectrum. Helium was discovered in the solar spectrum by Bunsen and Kirchoff using this technique. Hence the name derived from Helios for the Sun.
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.
Absorption of energy at atom energy levels cause the line spectrum.
Dark lines especially in solar spectrum have been named as Fraunhofer lines. These line are good examples for line absorption spectrum
dark-line spectrum...
wavelengths of absorbed or emitted photons
The wave lengths of lines of the spectrum are different for each chemical element.
The color in the flame is the representation of a specific line in the spectrum.
Yes , every element has different line in the spectrum.
The line spectrum is usually used to sort out the atomic fingerprint as the gas emit light at very specific frequencies when exposed to the electromagnetic waves. The electromagnetic waves are usually displayed in form of the spectral lines.
Wavelengths of absorbed or emitted photons Every line in a line spectrum is caused by a transition, from one quantum state to another quantum state, involving electrons.
There are several kinds of spectra. Bright line spectrum, or emission spectrum, is when light emitted by a gas has an electrical discharge going through it, and it produces a spectrum of just a few isolated parallel lines.
Because the spectra of elements is determined by the energy of transitions of electrons between two allowed quantum states. Since these energy differences can have only certain specified values, the spectrum consists of lines: The spectrum frequency values intermediate between the lines do not correspond to transitions between any two allowed quantum states and therefore do not appear in the spectrum
An absorption spectrum can tell the astronomer or physicist what elements are in the starlight being observed. A diffraction grating is used to split the incoming light into a spectrum of colors. Sodium, for example, causes dark Fraunhofer lines at known points in the visible spectrum. Helium was discovered in the solar spectrum by Bunsen and Kirchoff using this technique. Hence the name derived from Helios for the Sun.