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What causes the Balmer Jump? - Astronomy Stack Exchange To quote Wikipedia: Balmer Jump is caused by electrons being completely ionized directly from the second energy level of a hydrogen atom (bound-free absorption), which creates a continuum absorpti
In galaxy optical spectra, why are Hbeta and Hdelta sometimes . . . From Wikipedia, Balmer lines are usually emission lines in the spectra of spiral and irregular galaxies probably due to the presence of type A stars If ellipticals lack hot (O, B and A type?) stars, and are gas poor (?), then is it the remaining stars doing the absorbing? Also, are the CaII-H and -K doublet ever emission lines?
How does one estimate the mass of a galaxy using the Balmer break region? I was wondering if someone could detail how the Balmer break region is used to determine galaxy mass estimates (and perhaps the dependence on redshift i e what redshifts is this technique most feasible and why and also how using near-infrared data plays a role in this)
spectroscopy - Why is He I 6678. 151 line used for investigating . . . Neutral Hydrogen exhibits a Balmer series which is a transition of the electron from a higher energy level down to the n=2 energy level The n=3 to n=2 transition, otherwise known as Ba-α has a wavelength of 6562 79 Angstroms Neutral Helium (a k a He I) can exhibit emissions similar to the Hydrogen Balmer series And in fact, the He I 6678 151 Angstrom emission line is closest in energy to
the sun - Helium in solar spectra - Astronomy Stack Exchange You can argue it from an order of magnitude that the lower levels of visible transitions in helium are about 20 eV above the ground state, compared with 10 2 eV for the hydrogen Balmer lines In other words, for visible hydrogen absorption lines you need to have a population of atoms excited to a level 10 2 eV above the ground state
Using emission lines to determine redshift of a quasar I am attempting this past paper question and am not sure how to tackle this, this is not homework! :) The spectrum of a distant quasar shows two broad emission lines with observed wavelengths o
the sun - Why are the solar prominences visible during a total solar . . . Structures that are seen in emission off the photospheric limb of the Sun - know as prominences - are emitting a lot of light at the specific wavelength of the Balmer H α α line at 656 nm and these tend to appear "pink-ish" (when the Sun is completely obscured by the Moon), which is a mixture od direct red light from the prominence and white
Nebula and its colors - Astronomy Stack Exchange Generally speaking, green colours in a nebula are due to forbidden transitions in ionised Oxygen, though can feature the hydrogen β β Balmer line Red colours can be due to Hydrogen α α, but there are also lines due to ionised sulphur and nitrogen that often make contributions