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Topic: Paschen series

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Balmer series

Lyman series

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	BIGS, physics: Spectral series of hydrogen
		From the Lyman series to the Brackett series, it can be seen that the energy applied forces the hydrogen electrons to a higher energy level by a quantum leap.
		The Paschen series becomes visible if the electron first falls to an excited state with the principal quantum number of n = 3 before returning to its initial state.
		The lines of the Paschen series (n = 3) are located in the near infrared range of the spectrum.
	www.bigs.de /en/shop/htm/termsch01.html (638 words)

	Search Encyclopedia.com
		electromotive series electromotive series, list of metals whose order indicates the relative tendency to be oxidized, or to give up electrons (see oxidation and reduction); the list also includes the gas hydrogen.
		Members of the series are often called lanthanides, although lanthanum (atomic number 57) is not always considered a member of the series.
		series series, in mathematics, indicated sum of a sequence of terms.
	www.encyclopedia.com /searchpool.asp?target=@DOCTITLE+series (230 words)

	spectrum. The Columbia Encyclopedia, Sixth Edition. 2001-05
		It consists of a series of dark lines superimposed on a continuous spectrum, each line corresponding to a frequency where a bright line would appear if the gas were incandescent.
		The Fraunhofer lines appearing in the spectrum of the sun are an example of a dark-line spectrum; they are caused by the absorption of certain frequencies of light by the cooler, outer layers of the solar atmosphere.
		In his 1913 model of the hydrogen atom Niels Bohr showed that the observed series of lines could be explained by assuming that electrons are restricted to atomic orbits in which their orbital angular momentum is an integral multiple of the quantity h/2
	www.bartleby.com /65/sp/spectrum.html (676 words)

	Encyclopedia: Excited state (Site not responding. Last check: 2007-10-23)
		Emission of photons from atoms in various excited states leads to an electromagnetic spectrum showing a series of characteristic emission lines (including, in the case of the hydrogen atom, the Lyman series, the Balmer series, the Paschen series, the Brackett series.) The electromagnetic spectrum is the range of all possible electromagnetic radiation.
		A spectral line is a dark or bright line in an otherwise uniform and continuous spectrum, resulting from an excess or deficiency of photons in a narrow frequency range, compared with the nearby frequencies.
		The Lyman series is the series of transitions and resulting emission lines of the hydrogen atom as an electron goes from n ≥ 2 to n = 1 (where n is the principal quantum number referring to the energy level of the electron).
	www.nationmaster.com /encyclopedia/Excited-state (838 words)

	Brackett (1922) on his series
		Balmer series might be attributed to increasing the probability of transitions between the orbits of higher quantum numbers.
		All atoms which contribute to the radiation of the first Paschen line are left necessarily with the electron in the third orbit, whence it must proceed either to the second or the first orbit unless it is ejected to some orbit of greater quantum number by inelastic collision.
		It should be noticed that the higher members of the Paschen series occur in a region readily studied by photographic methods, plates hypersensitized by means of dicyanin being sensitive to 1.0 µ.
	dbhs.wvusd.k12.ca.us /webdocs/Chem-History/Brackett-1922/Brackett-1922.html (1916 words)

	POTW09 (Site not responding. Last check: 2007-10-23)
		The Balmer series of lines are shown in the figure above, and four of the lines in the series (the rightmost four lines) appear in the visible portion of the electromagnetic spectrum.
		The other lines in the series are in the ultraviolet region and are not visible to the human eye.
		Paschen series - transitions from higher shells to the M (n=3) shell.
	www2.yk.psu.edu /~jhb3/potw09.htm (531 words)

	Balmer's Formula
		Later, other researchers found that the series could be extended into ultraviolet wavelengths; the same formula still worked, with larger values of n.
		You can see that the series has a limit-- that is, as n gets larger and larger, the wavelength gets closer and closer to one particular value.
		For example, the Lyman series, which is entirely in the ultraviolet, fits the equation
	www.colorado.edu /physics/2000/quantumzone/balmer.html (362 words)

	The Bohr Atom
		The highest energy series of the emission spectrum matches the absorption spectrum and is called the Lyman series.
		The next series (with a similar pattern) is in the visible and ultraviolet region and is called the Balmer series.
		The Paschen series is in the infrared region.
	www.tannerm.com /bohratom.htm (855 words)

	atomic hydrogen emission spectrum
		If you now look at the Balmer series or the Paschen series, you will see that the pattern is just the same, but the series have become more compact.
		The Paschen series would be produced by jumps down to the 3-level, but the diagram is going to get very messy if I include those as well - not to mention all the other series with jumps down to the 4-level, the 5-level and so on.
		The problem is that the frequency of a series limit is quite difficult to find accurately from a spectrum because the lines are so close together in that region that the spectrum looks continuous.
	www.chemguide.co.uk /atoms/properties/hspectrum.html (2642 words)

	Paschen series -- Facts, Info, and Encyclopedia article (Site not responding. Last check: 2007-10-23)
		Paschen series -- Facts, Info, and Encyclopedia article
		The transitions are named sequentially by Greek letter: n = 4 to n = 3 is called Paschen-alpha, 5 to 3 is Paschen-beta, 6 to 3 is Paschen-gamma, etc.
		They are named after the (additional info and facts about Austro) Austro- (A person of German nationality) German physicist (additional info and facts about Friedrich Paschen) Friedrich Paschen.
	www.absoluteastronomy.com /encyclopedia/p/pa/paschen_series.htm (110 words)

	Atomic Physics
		Further experiments determined that there were additional, similar series of spectral lines produced by hydrogen in the infrared and ultraviolet regions.
		These series of lines could be described by equations similar to Balmer's.
		These lines in the Lyman series have wavelengths from 91 nm to 122 nm.
	www.ux1.eiu.edu /~cfadd/1160/Ch29Atm/Spect.html (266 words)

	Erik's Chemistry: Chapter 7: Electronic Structure of Atoms (Site not responding. Last check: 2007-10-23)
		By absorbing energy, it moves to a higher orbit of larger radius; energy is given off as light (photons) when the electron returns.
		The fixed radii was based on spectroscopy; Lyman Series (ultraviolet), Balmar Series (visible light), Paschen Series (infrared)
		The letters come from the atomic spectrum series from the 20th century.
	eppe.tripod.com /elstruct.htm (712 words)

	Astron. Astrophys. 324, 699-703 (1997) (Site not responding. Last check: 2007-10-23)
		The Paschen decrement as a density indicator in MWC349
		We present new observations of the Paschen series hydrogen recombination lines in the circumstellar shell of MWC349.
		The good agreement over a large range of n between the observed and the theoretical Paschen decrement shows that any departure from standard recombination theory, possibly due to the strong IR radiation field of the circumstellar disk, must be small.
	aa.springer.de /bibs/7324002/2300699/small.htm (169 words)

	[No title] (Site not responding. Last check: 2007-10-23)
		The Paschen and Brackett series exhibit a qualitatively similar behaviour, but the ``emission domain'' is at a higher column mass: log(m)> -.4.4 g cm$^{-2}$, log(M)> -4.2 g cm$^{-2}$ and log(M)> -3.8g cm$^{-2}$ respectively for the Balmer, Paschen and Brackett series.
		In opposition with other series, the Lyman lines show a monotonous decrease and even change to absorption for very low density models.
		All Hydrogen series, except the Lyman series for intermediate and high pressures, are sensitive to the temperature minimum when large changes are considered.
	star.arm.ac.uk /~ambn/abstract180.html (397 words)

	Remote Sensing Tutorial Page A-7 (Site not responding. Last check: 2007-10-23)
		Now, in more detail: Each element has a series of spectral lines that are diagnostic, being found in fixed locations in a spread of the spectrum as determined by the wavelengths of emitted radiation resulting from excitation of electrons into higher energy levels (recall the formula: ΔE = hν).
		For the Balmer series, the reverted level is N = 2; the Paschen series, N = 3.
		The Lyman series occurs in the Ultraviolet and the Paschen series in the near Infrared segments of the EM spectrum.
	rst.gsfc.nasa.gov /Sect20/A7.html (4692 words)

	Emission spectrum
		Transitions ending up at the n = 2 level give rise to photons in the Balmer series, which is light in the visible part of the electromagnetic spectrum.
		Transitions to the n = 1 level give rise to the Lyman series, and to the n = 3 level give the Paschen series.
		Such series of distinct spectral lines are observed experimentally when a gas such as hydrogen is heated up - the added heat energy excites the electrons, which subsequently fall into lower energy levels, emitting photons of various energies and, thus, light of various frequencies.
	theory.uwinnipeg.ca /mod_tech/node151.html (333 words)

	Rydberg formula - Wikipedia, the free encyclopedia
		run from 2 to infinity, the spectral lines known as the Lyman series converging to 91nm are obtained, in the same manner:
		The Lyman series is in the ultraviolet while the Balmer series is in the visible and the Paschen, Brackett, Pfund, and Humphreys series are in the infrared.
		The formula above can be extended for use with any hydrogen-like chemical elements.
	en.wikipedia.org /wiki/Rydberg_formula (250 words)

	Recitation #3: Using A Spreadsheet #1 (Site not responding. Last check: 2007-10-23)
		The Bohr Energy Level equations can be used in a spreadsheet to calculate the energies, frequencies and wavelengths of the various spectral lines that are possible in the various spectral series of hydrogen.
		The Paschen series, i.e., the final state is the n = 3 state
		At the bottom of the page, type in some information about where the various spectral lines in the three series occur with respect to visible light.
	www.physics.csbsju.edu /RPEG/213/handouts/R_3-2.bohr.spreadsheet.html (269 words)

	Ch 445 Balmer Series of Hydrogen
		By measuring the wavelength for several transitions, it is possible to determine the energy corresponding to those transitions and, hence, the Rydberg constant for the hydrogen atom.
		Transitions that share a common lower state appear to be organized into a series of lines that converge to a limiting wavelength.
		The convergence limit of the Paschen series is in the red part of the spectrum at about 820 nm, and all other series will appear in the infrared and beyond.
	www.sou.edu /chem/ch445/balmer.htm (1808 words)

	Paschen series - Wikipedia, the free encyclopedia
		The Paschen series is the series of transitions and resulting emission lines of the hydrogen atom as an electron goes from n ≥ 4 to n = 3 (where n refers to the energy level of the electron).
		They are named after the Austro-German physicist Friedrich Paschen.
		This page was last modified 20:26, 3 November 2005.
	en.wikipedia.org /wiki/Paschen_series (102 words)

	Spectral Classification of Stars
		Absorption lines caused by electrons starting in the n = 2 level are a part of the Balmer series, and those caused by electrons starting in the n = 3 level are a part of the Paschen series.
		The electron transitions that correspond to the first four absorption lines of the Lyman series are drawn for you as well as their identifying wavelengths (i.e.
		Astronomers call this particular absorption line H a (because it is the first line in the Balmer series and a is the first letter of the Greek alphabet), and it is created when an electron moves from the 2 nd to the 3 rd energy level.
	www.astro.washington.edu /labs/clearinghouse/labs/word_documents/classifying_stars.html (2164 words)

	Balmer spectral series: teaching notes
		Accounting for these regularities in the spectrum of hydrogen was an important aspect of Niels Bohr's model of the hydrogen atom, which was itself an important precursor of quantum mechanical descriptions of atomic structure.
		Balmer's speculation that there were other series of spectral lines for hydrogen was also correct; however, his extended formula (used here in exercise 3) did not quite predict their wavelengths correctly.
		The n=3 series begins with 9545 Å, in the infrared; it too was named after its discoverer, Friedrich Paschen.
	web.lemoyne.edu /~giunta/classicalcs/balmernote.html (257 words)

	Lyman series (Site not responding. Last check: 2007-10-23)
		The Lyman series is the series of transitions and resulting emission lines of the hydrogen atom as an electron goes from n ≥ 2 to n = 1(where n is the principal quantum number referring to theenergy level of the electron).
		Therefore, each wavelength of the emission lines corresponds to an electron dropping froma certain energy level (greater than 1) to the first energy level.
		The series is named after its discoverer, Theodore Lyman.
	www.therfcc.org /lyman-series-46887.html (410 words)

	The hydrogen lines (Site not responding. Last check: 2007-10-23)
		The Paschen series is written as Pa a
		The Lyman, Balmer and Paschen series are well separated in wavelength.
		The Balmer lines are in the optical, and the Paschen lines are infrared lines.
	iapetus.phy.umist.ac.uk /Teaching/IntroAstro/Hydrogen.html (212 words)

	Ch 01
		Electromagnetic radiation with a continuous spectrum of wavelengths, including those in the Lyman, Balmer, and Paschen series, enters one end of the tube and leaves the other end.
		When a photon, whose energy is equal to the energy difference for a transition in the Lyman series, is absorbed by a ground state electron, that electron will make a transition to a higher energy level.
		Although the absorption lines that correspond to transitions in the Lyman series are not present, there will be more absorption lines in the exiting radiation compared to the situation when the electrons are in the ground state, because absorption lines corresponding to both the Balmer and Paschen series will be present.
	www.emory.edu /PHYSICS/Faculty/Benson/142/concepts4/CQ30.htm (2154 words)

	U Budky -Be stars
		Infrared excess is interpreted as the contribution of the free-free radiation emitted in the ionized gas of the outer atmosphere and so it became an indicator of an extended atmosphere.
		This series is seen usually in absorption, except early type Be stars, where it may be in emission.
		If Paschen lines are in emission, the star has an infrared excess.
	www.asu.cas.cz /~andrea/be.html (1151 words)

	Lyman series (Site not responding. Last check: 2007-10-23)
		The Lyman series is the series of transitions and resulting emission lines of the hydrogen atom as an electron goes from n ≥ 2 to n = 1 (where n refers to the energy level of the electron).
		It has been known for some time that the radiation emmited from Hydrogen is non-continuous.
		Therefore, each wavelength of the emmision lines corresponds to an electron dropping from a certain energy level (greater than 1) to the first energy level.
	www.enlightenweb.net /l/ly/lyman_series.html (369 words)

	Erik's Chemistry: Chapter 7: Electronic Structure of Atoms (Site not responding. Last check: 2007-10-23)
		By absorbing energy, it moves to a higher orbit of larger radius; energy is given off as light (photons) when the electron returns.
		Electron returning to excited state (n=3) produce Paschen Series, infrared.
		The letters come from the atomic spectrum series from the 20th century.
	members.tripod.com /~EppE/elstruct.htm (712 words)

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