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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?
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
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)
2D Galaxy Spectrum taken by long-slit-spectrograph I have the 2D data (shape(1125,2058) taken by a long slit spectrograph, which looks as follows: The y-axis corresponds to the distance from the center, where the center is at the most bright green
Spectroscopy question about a Paschen series absorption There may be small amounts of Paschen and Balmer emission from the cloud via recombination Thus what you basically see is the spectrum of the star and since you aren't told what kind of star it is, then it's impossible to rule out the presence of emission lines or absorption lines of any kind
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 $\alpha$ 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
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
What is the origin of the OBAFGKM classification system? Once a body has been identified as a star it is classified into a subsection of either O,B,A,F,G,K or M (I think there are also 3 more letters recently added) What is the origin of this classifica