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	Balmer line - Wikipedia, the free encyclopedia
		A Balmer line is a hydrogen spectral line.
		The energies involved cause the Balmer lines to be in the optical spectrum.
		Balmer lines appear in a great variety of objects, hydrogen being the most common chemical element in the universe.
	en.wikipedia.org /wiki/Balmer_line (140 words)

	Balmer
		However, despite being a mathematics teacher and lecturer all his life, Balmer is best remembered for his work on spectral series and his formula, given in 1885, for the wavelengths of the spectral lines of the hydrogen atom.
		It is surprising to realise that Balmer was sixty years old when he wrote the paper for which he is famous on the spectral lines of the hydrogen atom and that he was seventy-two when he wrote his only other work on this topic.
		Putting m = 7 gave Balmer a predicted value for the next line and indeed a colleague at the University of Basel was able to tell Balmer that this line had been observed and the wavelength agreed with a high level of accuracy with the one Balmer's formula predicted.
	www-groups.dcs.st-and.ac.uk /~history/Mathematicians/Balmer.html (593 words)

	Balmer line (Site not responding. Last check: 2007-11-06)
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	www.serebella.com /encyclopedia/article-Balmer_line.html (525 words)

	The Balmer Formula
		At the time, Balmer was nearly 60 years old and taught mathematics and calligraphy at a high school for girls as well as giving classes at the University of Basle.
		Balmer was very interested in mathematical and physical ratios and was probably thrilled he could express the wavelengths of the hydrogen spectrum using integers.
		Balmer was devoted to numerology and was interested in things like how many sheep were in a flock or the number of steps of a Pyramid.
	dbhs.wvusd.k12.ca.us /webdocs/Electrons/Balmer-Formula.html (844 words)

	Balmer, Johann Jakob - Hutchinson encyclopedia article about Balmer, Johann Jakob
		Balmer was born near Basel, where he taught school for 40 years.
		In 1885 he published an equation that described the four visible spectral lines of hydrogen (all that were then known) and also predicted the existence of a fifth line at the limit of the visible spectrum, which was soon detected and measured.
		The five lines in the visible part of the hydrogen spectrum are now known as the Balmer series.
	encyclopedia.farlex.com /Balmer,%20Johann%20Jakob (290 words)

	Balmer line (Site not responding. Last check: 2007-11-06)
		The Balmer line s arise from transitions involving the second energy level and a higher level.
		The energies involved cause the Balmer line s to be in the optical spectrum.
		Balmer line s appear in a great variety of object, hydrogen being the most common chemical element in the universe.
	www.portaljuice.com /balmer_line.html (131 words)

	Line emission mechanisms (Site not responding. Last check: 2007-11-06)
		In addition, if the lines are produced near the white dwarf, one should expect to see high excitation absorption lines such as NV, CIV and SiIV in the ultraviolet (Fontaine and Michaud 1979, Vauclair 1979) as observed in G191-B2B (Bruhweiler and Kondo 1981).
		There are none of the broad emission lines typical of interacting binaries, such as those produced by an accretion disk or infalling gas close to the white dwarf surface.
		On the other hand, if line emission is due to reprocessing of the white dwarf EUV flux, then the variations in optical line intensity could also indicate underlying variations in the white dwarf EUV output.
	www.star.ucl.ac.uk /~cmj/thesis/node64.html (1265 words)

	The Balmer Relationship (Site not responding. Last check: 2007-11-06)
		In 1885 Johann Jacob Balmer (1825-1898) produces an empirical relationship between the four prominent lines in the hydrogen spectrum.
		Without having seen such a line, Balmer suggested that there should be one at the edge of the visible violet.
		Example Calculation: Using Balmer's original formula, calculate the wavelength of the wavelength of the line Balmer predicted at the edge of the violet.
	gemini.tntech.edu /~tfurtsch/scihist/balmer.htm (334 words)

	Johann Jacob Balmer (Site not responding. Last check: 2007-11-06)
		The wavelengths of the first four hydrogen lines are obtained by multiplying the fundamental number h = 3645.6 in succession by the coefficients 9/5; 4/3; 25/21; and 9/8.
		We may almost certainly assume that the other lines of the white stars which Huggins found farther on in the ultraviolet part of the spectrum will be expressed by the formula.
		Whether the hydrogen lines of the white stars agree with the formula to this point or whether other numerical relations gradually replace it can only be determined by observation.
	web.lemoyne.edu /~giunta/balmer.html (1120 words)

	Pictor A: Discovery of Strong Balmer Line Variations (Site not responding. Last check: 2007-11-06)
		We have detected strong changes in Balmer line flux and profile shape for the Broad Line Radio Galaxy Pictor A (0518--458).
		The Balmer lines observed in 1993 are reminiscent of the rare kind (extremely broad profiles with shifted ``humps'') observed in Arp 102B, 3C390.3 and a handful of other BLRGs.
		The emission line profile widths and redshift are consistent with emission from an inclined relativistic accretion disk but the relative strength of the red and blue ``humps'' are not.
	www.aas.org /publications/baas/v26n2/aas184/abs/S1103.html (253 words)

	Extinction of the optical emission line regions
		The relative ratios of the Balmer lines of hydrogen are often used as extinction indicators due to the fact that they are observationally convenient (being in the optical band), strong and their intrinsic relative flux ratios are fairly well determined from atomic theory.
		line were measured in different spectrographs, the data from which have undergone independent reduction and calibration.
		lines all appear in the data from the same spectrograph and so the two independent Balmer decrements that can be formed from these three lines are not sensitive to uncertainties in the overall normalization.
	www.astro.umd.edu /~chris/publications/html_papers/aat/node13.html (819 words)

	Comparison to optically-selected sample (Site not responding. Last check: 2007-11-06)
		The atmospheres I have used for the Balmer line modelling are all homogenous pure hydrogen DA atmospheres.
		The Balmer line profile fitting should be relatively unaffected and thus give a truer indication of the actual effective temperature in these cases (until improved atmospheric models become available).
		However, the model fitting of the Balmer line profiles to the FOS spectra turns out to be largely insensitive to the surface gravity determination, due to the low S/N and resolution of the spectra.
	www.star.ucl.ac.uk /~cmj/thesis/node40.html (2067 words)

	MSSL Extragalactic Astronomy - Population Studies
		The predicted FWHM of the composite profile of an arbitrary line, plotted as a function of the ILR/VBLR ratio, is shown in Figure (b).
		Looking at the Balmer lines, we find that the Halpha FWHM is also dependent on the X-ray slope, and increases as the X-ray slope hardens (shown opposite; the outlier highlighted by the square has double-peaked Balmer lines - it may contain a binary fl hole or line-emitting jets).
		This may be an orientation effect, consistent with the basic geometry of the Unified Model, or it may indicate that the position of the Balmer line region, relative to the central supermassive fl hole, depends on the amount of gas which lies beyond the central regions.
	www.mssl.ucl.ac.uk /www_astro/agn/agn_rixos.html (710 words)

	[48.09] Ionization Structure in the Narrow Line Region of M51 (Site not responding. Last check: 2007-11-06)
		Emission-line diagnostics as a function of projected radial distance are employed for nine emission-line clouds which extend 2.5\arcsec\ (102~pc) from the nucleus to examine the reddening, density, temperature, and ionization state of the NLR gas.
		Using the observed H\alpha/H\beta Balmer line ratio as a measure of the extinction in the NLR, we observe that the emission-line clouds closest to the obscured nucleus are generally more reddened than those at larger radii.
		The ionization state of the gas as probed by the [OII] 3727/[OIII] 5007 line ratio indicates that within the inner near-nuclear region (r \la 1\arcsec) the ionization decreases with increasing radius.
	www.aas.org /publications/baas/v34n4/aas201/1185.htm (338 words)

	[No title] (Site not responding. Last check: 2007-11-06)
		We obtain the Paschen lines in emission and Paschen decrements as large as 41 for Pa$_{\beta}$.
		High electron density and collisional control is a necessary condition to drive the Balmer lines into emission in M dwarf atmospheres.
		The total radiative cooling in the Hydrogen lines and continua is about 1.22 10$^8$ erg cm$^{-2}$ s$^{-1}$, of which 66\% arise from the Balmer series and continuum.
	star.arm.ac.uk /~ambn/abstract174.html (595 words)

	Balmer Formula Calculations (Site not responding. Last check: 2007-11-06)
		The four calculations shown below generate the wavelengths of the four visible lines of the hydrogen spectrum.
		This ends the visible lines of the hydrogen spectrum.
		However, with the Balmer formula, production of wavelengths was quite easy and, as techniques improved, each other series was discovered.
	dbhs.wvusd.k12.ca.us /webdocs/Electrons/Balmer-Formula-Calcs.html (170 words)

	Abstracts of accepted papers: (Site not responding. Last check: 2007-11-06)
		As the linear polarization is but weakly sensitive to the variations of the field modulus, we interpret the polarization anomalies in terms of inclination changes of the lines of force within their meridian plane.
		Line profile variations of the Fe II Zeeman doublet may be consistent with a dipole field whose pole-to-equator modulus ratio has been decreased by about 20%.
		4026 line equivalent width variations: however on the basis of atmosphere model calculations, we can exclude that light variations could be mainly due to the different helium abundance concentrations on the stellar surface.
	www.eso.org /gen-fac/pubs/apn/Archive/north/no25/N25/node3.html (2775 words)

	Atomic Absorption and Emission Spectra (Site not responding. Last check: 2007-11-06)
		Thus, for example, the Balmer Series involves transitions starting (for absorption) or ending (for emission) with the first excited state of hydrogen, while the Lyman Series involves transitions that start or end with the ground state of hydrogen; the adjacent image illustrates the atomic transitions that produce these two series in emission.
		The Balmer lines are designated by H with a greek subscript in order of decreasing wavelength.
		Thus the longest wavelength Balmer transition is designated H with a subscript alpha, the second longest H with a subscript beta, and so on.
	csep10.phys.utk.edu /astr162/lect/light/absorption.html (408 words)

	Astron. Astrophys. 347, 876-890 (1999) (Site not responding. Last check: 2007-11-06)
		The Balmer line profiles are a useful tool in investigating convection because they are very sensitive to the parameters of convection used in the stellar atmosphere codes.
		lines are formed at different depths in the atmosphere.
		lines are different, as expected, due to the differing levels of formation.
	aa.springer.de /papers/9347003/2300876/small.htm (302 words)

	Doppler-Free Saturated Absorption Spectroscopy
		Narrow line width, tunable lasers have revolutionized optical spectroscopy because of their unique ability to resolve closely spaced lines in optical spectra and thereby reveal some of the most subtle details of the underlying atomic and molecular structure.
		The sole purpose of the argon ion laser is to serve as a bright, highly collimated, blue-green light source to pump the Coherent 699-21 Ring Dye Laser, whose optical layout is shown schematically in Fig.
		The analogous Doppler broadening of emission lines is evident in the hydrogen Balmer line spectra of Expt.XII.
	www.breadnet.middlebury.edu /~PHManual/dopfree.html (3229 words)

	[No title] (Site not responding. Last check: 2007-11-06)
		The HeII 1640Å line is visible in the STIS spectrum which represents the first detection of trace He in an apparently isolated DA white dwarf.
		An important precursor to using the Lyman lines, particularly for those binaries where the white dwarf Balmer lines cannot be observed, is to establish that this technique gives reproducible results which are consistent with the Balmer line measurements of isolated stars.
		There seems to be good overall agreement between the Balmer and Lyman line measurements, although significant differences are found for a few stars, possibly arising from systematic effects in the observation and data reduction process.
	www.star.le.ac.uk /wd/report.htm (1784 words)

	Spectroscope and Line Spectra (Site not responding. Last check: 2007-11-06)
		Using a spreadsheet, calculate the frequency and energy for each line for each element.
		Compare your lines for the helium, hydrogen and mercury with those on the spectrum chart.
		Don't worry about the color in the green-yellow region, the color scale is off, but the wavelength values of the lines are okay.
	www.chem.vt.edu /RVGS/ACT/lab/Experiments/Exp_13-Spectra_Activity.html (188 words)

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	store.balmer.com (206 words)

	Balmer's Formula
		Balmer examined the four visible lines in the spectrum of the hydrogen atom; their wavelengths are 410 nm, 434 nm, 486 nm, and 656 nm.
		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.
		That's just what experimentalists saw; around 365 nm, the lines became too close together to distinguish.
	www.colorado.edu /physics/2000/quantumzone/balmer.html (363 words)

	Be stars / Scientific aims
		observations enable for the first time to study exactly simultaneous line-profile low-order variations from the near-UV and to near-IR spectral region and, thereby, of lines formed under the different physical conditions and at different locations in the (extended) atmospheres of Be stars.
		The test observations obtained in January - March 1995 prove, that the quality of the spectra is fully sufficient for this aim.
		The fl spectrum was taken during a phase of relative quiescence in April 1996, while the red spectrum shows the line during an active phase, a so-called outburst in May 1996.
	www.lsw.uni-heidelberg.de /users/triviniu/aims.html (542 words)

	Monthly Notices of the Royal Astronomical Society Abstract (Site not responding. Last check: 2007-11-06)
		The observation of the strengths and profiles of the hydrogen Balmer absorption series is an established technique for determining the effective temperature and surface gravity of hot H-rich white dwarf stars.
		We have already made a first attempt to study this problem, comparing Lyman line measurements from a variety of FUV instruments with ground-based Balmer line studies.
		The new results partially reproduce the earlier study, showing that Balmer and Lyman line determined temperatures are in good agreement up to ~50 000 K. However, above this value there is an increasing systematic difference between the Lyman and Balmer line results, the former yielding the higher temperature.
	www.blackwellpublishing.com /abstract.asp?ref=0035-8711&vid=344&iid=2&aid=26&s=&site=1 (563 words)

	[No title] (Site not responding. Last check: 2007-11-06)
		With the help of theoretically motivated disk illumination patterns and the resulting disk surface-emissivity, detailed studies of individual line shapes can constrain the disk inclination and the size of the line emitting region and distinguish between axisymmetric and non-axisymmetric disks.
		The distribution of model disk parameters inferred from the observed line profiles can be used to test AGN unification schemes and disk stability at large distance (few thousand to about ten thousand gravitational radii) from the central fl hole.
		Less than 3% of all z<0.33 AGN already surveyed (as of June 2002) had Halpha lines indicative of disk emission, but only about 1/4 of those (a total of 23 objects to date) were consistent with the simplest axisymmetric disk models, which allow unambiguous model fits.
	www.sdss.org /collaboration/strateva.txt (435 words)

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