Spectral Lines in Stars - Absorbtion and Emission
This spectral atlas contains a sample of the standard spectral type stars, peculiar stars, variable stars, and some special stars. OBAFGKM and more. The spectral types and sub-classes represent a temperature sequence, from hotter (O . Now we can start making the connection between the peaks and valleys we see in sequence of spectral types, OBAFGKM, is actually a temperature sequence. Color of a star depends on its Temperature: Red Stars are Cooler, Blue fusion of 4 Hydrogen into 1 Helium: Main Sequence stars "burn" Hydrogen into Can we use stellar spectra to distinguish among different types of stars? Left with 7 primary classes: O B A F G K M: Later work added the classes R, N, and S.
Although based on the absorption lines, spectral type tells you about the surface temperature of the star.Stars: Crash Course Astronomy #26
One can see that there are few spectral lines in the early spectral types O and B. This reflects the simplicity of atomic structure associated with high temperature.
Hertzsprung-Russell Diagram | COSMOS
While the later spectral types K and M have a large number of lines indicating the larger number of atomic structures possible at lower temperatures. Annie Cannon Image Source: The principal figure in this story was Annie Jump Cannon.
Pickering in the 's to participate in the classification of spectra. She quickly became very proficient at classification examining several hundred stars per hour. She completed a catalogue of spectral types for hundreds of thousands of stars. Three blackbody curves at different temperatures. Planck Curves The outward appearance of stars depends more strongly on the underlying continuous spectrum coming from the inner parts of a star than the absorption at its surface.
Continuous spectra for stellar interiors at different temperatures are described by Planck Curves shown in the figure to the left. Note that as the temperature increases the total amount of light energy produced the area under the curve increases and the peak wavelength the color at which the most light is produced moves to smaller more energetic wavelengths. Not all of the light will make it through.
All the photons that have exactly Likewise, no light with an energy of 1. The light that the hydrogen cloud absorbs shows up as dips in the cloud's spectrum.
Lecture 1: Stars: Masses, Luminosities, Tempertatures
If the cloud were too hot, however, all its hydrogen atoms will crash into each other with enough force to free their electrons, and the gas will become ionized. The hot cloud's hydrogen ions have no electrons, so they cannot absorb light.
When you look at the hot cloud's spectrum, you will not see any valleys from hydrogen absorption lines. Ionization occurs at about 10, K for hydrogen.
Therefore, if you do not see hydrogen lines in the hot cloud's spectrum, you can conclude it is hotter than 10, K. However, if the cloud were too cool, then the light would not have enough energy to boost its electrons into higher energy levels.
- Stellar classification
- Absorption and Emission Lines
- Spectral Classification of Stars
In this case, you also would not see any hydrogen lines in the cloud's spectrum. You would see the strongest hydrogen lines for a cloud that is at about K.