balmer series造句

• Designations from the early Balmer Series are in parentheses.
• The Bohr assumptions recover the observed Balmer series.
• The solution for the hydrogen atom describes standing waves of energy exactly given by the Balmer series.
• Rydberg managed to find a formula to match the known Balmer series emission lines, and also predicted those not yet discovered.
• Urey and grating spectrograph, a sensitive device that had been recently installed at Columbia and was capable of resolving the Balmer series.
• At the limit of the Balmer series a change happens where at shorter wavelengths more bound-bound Balmer series transitions cause more opacity.
• At the limit of the Balmer series a change happens where at shorter wavelengths more bound-bound Balmer series transitions cause more opacity.
• Urey and his colleague George Murphy calculated the redshift of heavy hydrogen from the Balmer series and observed very faint lines on a spectrographic study.
• I'm not entirely sure, but since 365.1nm is in the visible light spectrum that means it's in the Balmer series?
• Emission lines of hydrogen ( mainly of the Lyman series and Balmer series ), helium, carbon, magnesium, iron and oxygen are the brightest lines.
• The spectrum of WR 42e shows many characteristics of an OIf * star, such as hydrogen Balmer series absorption lines and emission lines of ionised nitrogen and helium.
• The visual spectrum of Vega is dominated by absorption lines of hydrogen; specifically by the hydrogen Balmer series with the electron at the n = 2 principal quantum number.
• The solution of this equation for atoms led to the explanation of the Balmer series for atomic spectra and consequently formed a basis for all of atomic physics and chemistry.
• Due to the prevalence of hydrogen in interstellar gas, and its relatively low energy of ionization, many emission nebulae appear red due to the strong emissions of the Balmer series.
• The spectral classification of stars, which is primarily a determination of surface temperature, is based on the relative strength of spectral lines, and the Balmer series in particular is very important.
• Emission spectra from W . M . Keck Observatory, obtained by Palomar Transient Factory indicate that this is a type II supernova with a relatively blue continuum with P Cygni profiles in the Balmer series.
• N III and N IV emission lines lines are stronger than N V, and He I lines are stronger than He II, The Balmer series hydrogen lines and some other lines have P Cygni profiles.
• The star appears, based on its spectrum in the Balmer series, to be a blue supergiant, although in reality it is an old low-mass star on the post-AGP phase of its life.
• The H ? emission is often unusually strong compared to other lines of the Balmer series in a normal M star, but this is due to the weakness of the TiO band that would otherwise dilute the H ? emission.
• The Balmer series is characterized by the electron transitioning from " n " e " 3 to " n " = 2, where " n " refers to the radial quantum number or principal quantum number of the electron.