My first few times out with a star spectroscope from Rainbow Optics filled my mind with unanswered questions. I was impressed with the prominence of the hydrogen lines in Vega, and amazed at the complexity of the spectra of Betelgeuse, but I wanted to understand what was going on. One of the best places I found for answers is Stars and Their Spectra by James Kaler, published by Cambridge University Press.
Here are some of my questions and a brief summary of the answers I found:
How are spectral lines formed?
By electrons jumping between different energy levels in the atoms in the starís outer layers. Bound electrons can absorb and emit energy only in certain discrete amounts. When an electron absorbs a photon of light with just the right amount of energy, it jumps to a higher level. When the electron spontaneously jumps back to a lower energy level, a photon is emitted. Enough electrons jumping between any two given energy levels of a certain element will result in a spectral emission or absorption line at a characteristic wavelength.
For example, the strongest spectral line in a hot main-sequence star like Vega lies in the blue-green part of the spectrum where our eyes are most sensitive to light. It is a dark or absorption line resulting from large numbers of electrons jumping from the second to the fourth energy level of the neutral hydrogen atom, and is known as hydrogen beta (in the Balmer series.)
Why do I see dark absorption lines rather than bright emission lines?
Gas under high pressure produces a continuous spectrum, a rainbow of colors. Continuous radiation viewed through a low density gas results in an absorption-line spectrum. Whatís happening here is that radiation emitted by gas under high pressure deep within the star is being absorbed by low density gas in the starís outer layers.
What kinds of deep sky objects have emission-line spectra?
A low density gas shows an emission-line spectrum, when not observed against a background of continuous radiation. Thus emission lines are found in the spectra of planetary and diffuse nebulae, and in some peculiar stars. In the latter case the lines often arise from gas clouds ejected from the star by strong stellar winds.
Vega and Deneb are both A-type stars, yet the prominent hydrogen lines of Vega are missing in the spectra of Deneb. Why?
All spectral lines have a certain width, caused by atomic collision perturbing the energy levels, which permits the atoms to absorb light slightly away from the line center. Generally, the greater the pressure and density of the gas, the broader and more prominent the lines will be.
Vega is a main-sequence or dwarf star, Deneb a supergiant. At the relatively low pressure and density typical of the outer layers of supergiants, atomic collisions are relatively rare and the spectral lines are consequently much narrower and less prominent than in dwarfs.
Why are the hydrogen lines weaker in cooler stars?
At cooler temperatures most electrons are in the ground state, at the the lowest energy level, because of the relatively few atomic collisions. Jumps to and from the ground state of neutral hydrogen produce spectral lines in the Lyman series, the strongest of which fall in the ultraviolet part of the spectrum, where we canít see them. In cooler stars the relative scarcity of electrons at higher energy levels results in weaker absorption lines in the Balmer series, visible to the human eye.
Why do spectral lines from metals become more prominent with decreasing temperature?
At cooler temperatures fewer elements are ionized, i.e., have lost one or more electrons through atomic collisions. Spectral lines from neutral (and many singly-ionized) elements tend to fall into the visual part of the spectrum, whereas lines from more highly ionized atoms fall in the ultraviolet. (Metals are elements heavier than hydrogen and helium.)
What are the thick bands in the spectra of cool stars like Betelgeuse?
These bands arise from molecules, most commonly titanium oxide. They are formed in a manner similar to but much more complex than atomic spectra. In addition to the atomic energy levels, in a molecule there are also vibrational and rotational states to be accounted for. The collection of jumps between the various atomic, vibrational and rotational states of a molecule, in all their combinations, results in a series of lines converging toward a characteristic wavelength known as the band head. The spectra of red carbon stars display similar banding, this time from carbon molecules.
Why are these bands absent in hot stars?
Stable molecules cannot form in the conditions of high pressure and density typical of the outer layers of hot stars because of the frequent atomic collisions.