Main Sequence Rules: Definition & Interpretation

In summary, when viewing an HR diagram, the main sequence curve is apparent, but it's unclear which stars should be considered main sequence. There is room for interpretation when it comes to which stars should be considered main sequence. Regarding the shaded area, it's unclear which stars should be considered main sequence, but it's probably the right ballpark.
  • #1
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When viewing an HR diagram, the main sequence curve is apparent, and the general shape of it is obvious. However, in this truncated version, it's unclear to me exactly which stars should be considered main sequence. I've added a shaded grey area as what I think I should count as main sequence, but there's a bit of room for interpretation. Are there hard-and-fast rules, or is it a matter of opinion? What do you think of this shaded area?
reddit help hr diagram.PNG
 
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  • #2
There are two possible definitions of the main sequence, one is empirical and is the luminosity class V, but more commonly the definition is physical rather than empirical-- it is stars that are fusing hydrogen in their core. So if we take the latter meaning, the "subgiants" that are between the main sequence and the red giant branch have stopped core fusion and are instead fusing in small shells around an inert core, but the core is not yet tiny and degenerate. As the core shrinks further and goes degenerate, the shell gets really tiny and even higher in temperature, and the envelope will puff out and the star will move up and to the right into the giant branch. So I think you'd have to use interior models to decide where the main sequence ends and the subgiants begin, but your shaded area is probably the right ballpark.

Another key point to bear in mind is that many stars are actually double or triple stars, and this normally cannot be determined with certainty when the stars are plotted on the H-R diagram, unless you can separate the spectra based on their Doppler shifts for "spectroscopic" binaries (close binaries seen not from above the orbits). So you can get points that are actually a kind of average of different stellar types, creating confusion as to exactly what type of star you are looking at.
 
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  • #3
Slightly OT: IIRC, a bunch of 'weird' Hipparchos distances have been attributed to orbital motion of unresolved binaries skewing the measured parallax. Some 'oops' seem due to mega-flares offsetting the nominal positions...

As mentioned above, spectroscopic binaries aligned such their orbital Doppler shifts are masked by surface activity are complex targets. Worse, contamination by mass-transfer or merger may skew determinations...

Must be said, watching such riddles and apparent paradoxes being patiently un-picked is excellent sport !
 

FAQ: Main Sequence Rules: Definition & Interpretation

1. What is the main sequence in astronomy?

The main sequence is a continuous band of stars on the Hertzsprung-Russell diagram that represents the majority of stars in the universe. It is the stage of a star's life cycle where it is fusing hydrogen into helium in its core, and it is the longest and most stable stage of a star's life.

2. What are the main sequence rules?

The main sequence rules are a set of guidelines used to interpret the position of a star on the Hertzsprung-Russell diagram. They state that the luminosity of a star is directly proportional to its mass, and that the temperature of a star is directly proportional to its color. Additionally, the main sequence rules also state that as a star's mass increases, its lifetime decreases.

3. How are main sequence stars classified?

Main sequence stars are classified based on their spectral type, which is determined by their surface temperature. The most common spectral types for main sequence stars are O, B, A, F, G, K, and M, with O being the hottest and M being the coolest. These spectral types are further divided into subcategories, such as O1-O9 and M0-M9, with the number indicating the specific temperature within the range.

4. What is the significance of the main sequence?

The main sequence is significant because it provides a way for astronomers to categorize and understand the vast majority of stars in the universe. It also allows for the prediction of a star's properties, such as its size, temperature, and lifetime, based on its position on the Hertzsprung-Russell diagram. The main sequence also serves as a benchmark for comparing and studying different types of stars.

5. Can a star leave the main sequence?

Yes, a star can leave the main sequence when it exhausts its supply of hydrogen fuel in its core. This typically happens when a star reaches the end of its main sequence lifetime, which can range from millions to billions of years depending on its mass. Once a star leaves the main sequence, it will enter a new stage of its life cycle, such as becoming a red giant or a white dwarf.

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