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A spectral line is choose a fingerprint that deserve to be used to identify the atoms, elements or molecules present in a star, galaxy or cloud of interstellar gas. If we sepaprice the incoming light from a celestial source making use of a prism, we will frequently watch a spectrum of colours crossed with discrete lines. Keep in mind that spectral lines can additionally happen in other areas of the electromagnetic spectrum, although we can no longer use a prism to help determine them.

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There are 2 forms of spectral lines in the visible part of the electromagnetic spectrum:


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Emission lines are viewed as coloured lines on a black background.
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Absorption lines are viewed as babsence lines on a coloured background.

The visibility of spectral lines is described by quantum mechanics in regards to the power levels of atoms, ions and molecules. These energy levels depfinish on the numbers of prolots, electrons and also neutrons in an atom, and also the limited collection of configurations in which these elepsychological pwrite-ups deserve to exist (the collection of quantum numbers). Atoms favor to be in their ground state, wright here every one of the electrons are located as close to the nucleus as feasible. Absorption lines occur as soon as an atom, aspect or molecule absorbs a photon with an power equal to the difference in between 2 power levels. This causes an electron to be promoted right into a higher power level, and the atom, element or molecule is shelp to be in an excited state. Emission lines occur as soon as the electrons of an excited atom, aspect or molecule relocate between energy levels, returning in the direction of the ground state.

The spectral lines of a certain facet or molecule at remainder in a laboratory constantly take place at the very same wavelengths. For this reason, we are able to determine which element or molecule is leading to the spectral lines. If the emitter or absorber is in motion, however, the position of the spectral lines will be Doppler shifted alengthy the spectrum. A redshift (spectral lines relocate to much longer wavelengths) occurs for an emitter/absorber relocating away from the observer, while a blueshift (spectral lines relocate to shorter wavelengths) corresponds to motion in the direction of the observer.

Spectral lines might additionally be broadfinished by:

Collisional Broadening: as a result of interactions through adjoining atoms, ions or moleculesZeemale Splitting: wright here power levels are break-up right into sub-levels by a magnetic area.

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The Hesitation Principle also provides a herbal expanding of all spectral lines, through a organic width of Δν = ΔE/h ≈ 1/Δt wright here h is Planck’s consistent, Δν is the width of the line, ΔE is the equivalent spcheck out in power, and t is the life time of the energy state (commonly ~10-8 seconds).