Talk:Spectral line

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Oldest comment

Does anyone know how easy it is to see these spectral lines? For instance, if I have a simple prism and I use it to see the sun's spectrum, can I observe a few lines with the naked eye?

Looking at the sun, probably not, but looking at a high-intensity street light, you certainly can see the lines of the evaporated metals in the lamp.Paul Reiser 01:11, 23 Dec 2004 (UTC)

Zeeman Effect

What about the Zeeman Effect on spectral lines? Korandder 09:24, 1 August 2007 (UTC)[reply]

Isomer shift

Isomer shift is the displacement of an absorption line due to the absorbing nuclei having different s-electron densities from that of the emitting nuclei.

Shouldn't that paragraph be in the section below that's about broadening and shifting? It seems very out of place where it is.

Also I don't understand what it's saying. It needs more explanation. — Preceding unsigned comment added by 64.50.84.194 (talk) 00:38, 13 April 2006

Photon Cascade

The revision by 84.194.165.197 read:

...photon is absorbed. Then it will be spontaneously re-emitted, either in the same frequency as the original or in a cascade (even multiple of the original photon frequency), where the sum of the energies of the photons emitted will be the same as the energy of the one absorbed.

This can't be right. If the sum of the energies of the emitted photons equals the energy of the original photon, then each of those energies must be less than the energy of the original photon. The energies (and therefore the frequencies) of the emitted photons can't be even multiples of the original photon energy or frequency. I don't know enough about photon cascades to correct this statement, however, so I hope 84.194.165.197 will correct it. Paul Reiser 18:42, 8 Jan 2005 (UTC)

collision broadening

isn't there missing something? I tought collision broadening was the predominant effect in all chaotic light sources e.g. in spectral lamps. (see Loudon, R: The Quantum Theory of Light. 3rd edn. Oxford Science, 2000. p. 76: "The dominant effects in the majority of experiments are the Doppler and collision broadening, and the latter is used (...) to model the typical features of a chaotic light source.") Or is this an article about plasma-related stuff only? any comments? —The preceding unsigned comment was added by Joerglwitsch (talk • contribs) 13:32, 19 February 2007 (UTC).[reply]

Gaussian broadening

A couple of articles mention Gaussian broadening and there seem to be a fair number of papers which mention the term. Should this be included in the list here? --Salix alba (talk) 21:55, 6 April 2007 (UTC)[reply]

I think this means any broadening mechanism which produces a Gaussian lineshape. Doppler broadening gives a Gaussian profile, as does natural broadening. Broadening is better classified by the physical phenomenon which causes it rather than the lineshape it produces. PAR 08:09, 7 April 2007 (UTC)[reply]

Thanks for that. I've changed Gaussian broadening appropriately. --Salix alba (talk) 09:45, 7 April 2007 (UTC)[reply]

I'm a bit mystified by this discussion. In chemistry a Gaussian line-shape(or something close to it) is common, for example in UV/vis spectra of compounds in solution. Furthermore, in decomposing a composite spectral band into component bands all sorts of line shapes have been used including Gauss-Lorentz sum and product funtions. There is also the fact that an observed line shape is a convolution of the "true" line-shape with an instrumental function, such as the finite slit function. Maybe there should be a separate article on line-shape, from the experimentalist's point of view, while this article concentrates on physical mechanisms of line-broadening? Petergans 08:43, 8 April 2007 (UTC)[reply]

Stuff

A new spectral line intensity formula for optical emission spectroscopy was presented by Dr:s Bo Thelin (experimental physicist) and Sten Yngström (theoretical physicist) at the beginning of the 1980:s. This formula has shown very good agreement between experiments (Ref 1) and the new theory (Ref 2). These references are summaries of earlier papers.

I = K \ left (frac { v^2 }{ c^2 }\ right ) \ e^left (\ frac { -J}{ k \ T \ right )} \ \ left (\ e^left ( \ frac { h \ v }{ k \ T \right - \ 1)^-1

K includes transition rates and element concentrations I= spectral line intensity, v= frequency , J=ionization energy and T=temperature

Many independent experimental methods strongly support the new formula, while the standard intensity formula with the Boltzmann term (upper energy level), deviates very much from experiments. Ref 1 Yngström,S. and Thelin,B. Applied Spectroscopy, 44, 1566, (1990) Ref 2 Yngström,S. International Journal of Theoretical Physics,Vol.33, No 7,(1994)--79.138.179.27 (talk) 21:40, 10 March 2008 (UTC)[reply]

Doppler Broadening

I think the section on Doppler Broadening could be stated a little more clearly. It says that the motion of particles causes a Doppler shift of the emitted radiation. The section then switches to talking about the bulk effects of this, which results in broadening and no shift. I don't think the transition from the single particle to bulk effects was clearly noted. I read it three times before I understood what it meant in saying it causes a shift and doesn't cause a shift. --TonyB 2005/05/02 —The preceding unsigned comment was added by 128.233.98.29 (talk) 15:14, 2 May 2007 (UTC).[reply]

Please proofread!

Added a stubby nomenclature section, please proofread, correct and enhance! I'm not anything near a physicist. For example I know of so called forbidden lines such as [OIV] that occur in planetary nebulae. Said: Rursus (☻) 07:09, 15 October 2008 (UTC)[reply]

Merge with atomic spectral line?

Oppose - molecules also have spectral lines. I suggest expanding both articles and making that point clear. --Kkmurray (talk) 23:11, 4 December 2012 (UTC)[reply]

Oppose - both articles need considerable attention, but I don't believe merging them together will improve anything. I believe this article is largely on topic for the topic while the current atomic spectral line article should be renamed since the content does not match the title. ronningt (talk) 01:48, 5 December 2012 (UTC)[reply]

List of spectral-line names

Should the list of named spectral lines (ED: specifically Fraunhofer lines) currently in the Abbe number article be added to this article? --SoledadKabocha (talk) 03:31, 25 November 2014 (UTC)[reply]

I suggest including links out to specific lists of named spectral lines within the naming section. However, I don't think those lists should be included here. Since this article is aiming to be broad, I think it needs a general introduction to nomenclature. These lists of named lines is one historical approach but not the only that is relevant to this article. ronningt (talk) 12:53, 26 November 2014 (UTC)[reply]

Reflection from gas

Absorption lines are produced even during reflection from an illuminated cold gas, as after reflection there is still the opportunity for a selective absorption (and re-scatter) between the point of reflection and the detector.

(1) What are some familiar or lab examples where light gets reflected from a cold gas?

(2) If the absorption occurs after the reflection, why do we bother to mention the reflection?

The description "reflection from an illuminated cold gas" seems to correspond to some established situation that is being inadequately presented. 89.217.11.36 (talk) 10:25, 22 February 2015 (UTC)[reply]

Thank you for drawing attention to this. I think this sentence was drawing attention to a very narrow age and was confusing the explanation in the process. I've edited that section. Please take a look. ronningt (talk) 20:36, 22 February 2015 (UTC)[reply]

Snowclone

It appears that physicists pay the same rapt attention to the telltale details of spectral line broadening as a hunter does to a trace of wind-blown sand in a hoof spoor. 89.217.11.36 (talk) 10:55, 22 February 2015 (UTC)[reply]

Incorrect image for tungsten's spectrum

Tantalum's spectrum is displayed next to tungsten. I don't know how to fix it - adding to this talk page is hard enough ;-) 76.167.219.69 (talk) 03:09, 28 September 2017 (UTC)[reply]

thanks! The tantalum image was used twice, a typo. Fixed. Thanks for the notice. -DePiep (talk) 05:00, 28 September 2017 (UTC)[reply]

Also assumed to be equatorial?

This is the spectrum of a blue sky somewhat close to the horizon, pointing east at around 3 or 4 pm (i.e., Sun toward the west) on a clear day.

It must at some level be presumed non-polar, because the poles don't even have east / west. At least the tropics? — MaxEnt 16:59, 16 October 2018 (UTC)[reply]

A Commons file used on this page or its Wikidata item has been nominated for deletion

The following Wikimedia Commons file used on this page or its Wikidata item has been nominated for deletion:

Mercury spectrum visible.png

Participate in the deletion discussion at the nomination page. —Community Tech bot (talk) 15:07, 6 April 2020 (UTC)[reply]

Mercury spectrum is missing in the table.

There is corrected version image of Mercury spectrum available (atomic number 80). https://commons.wikimedia.org/wiki/File:Mercury_spectrum_visible.png.

The older version was duplicate of https://commons.wikimedia.org/wiki/File:Barium_spectrum_visible.png,

so it was deleted as I understood from https://commons.wikimedia.org/wiki/Commons:Deletion_requests/File:Mercury_spectrum_visible.png.

The new version is obviously different. I do not know how to incorporate it into the table https://en.wikipedia.org/wiki/Template:Spectral_lines_of_the_elements 90.177.43.233 (talk) 07:37, 18 June 2022 (UTC)[reply]