MASON ASTR 113 - Stellar Evolution: After the Main Sequence

Unformatted text preview:

Stellar Evolution: After the Main SequenceGuiding QuestionsA star’s lifetime on the main sequence is proportional to its mass divided by its luminosity When core hydrogen fusion ceases, a main-sequence star becomes a red giantRed GiantsAs stars age and become giant stars, they expand tremendously and shed matter into space After the helium flash, a low-mass star moves quickly from the red-giant region of the H-R diagram to the horizontal branchThe cluster’s age can be estimated by the age of the main-sequence stars at the turnoff point (the upper end of the remaining As a cluster ages, the main sequence is “eaten away” from the upper left as stars of progressively smaller mass evolve into rePopulations (generations) of starsVariable StarsThere is a direct relationship between Cepheid periods of pulsation and their luminositiesMass transfer can affect the evolution of close binary star systemsGas flowing from one star to the other passes across the inner Lagrangian pointThis mass transfer can affect the evolutionary history of the stars that make up the binary systemKey WordsStellar Evolution:After the Main SequenceChapter Twenty-OneGuiding Questions1. How will our Sun change over the next few billion years?2. Why are red giants larger than main-sequence stars?3. Do all stars evolve into red giants at the same rate?4. How do we know that many stars lived and died before our Sun was born?5. Why do some giant stars pulsate in and out?6. Why do stars in some binary systems evolve in unusual ways?A star’s lifetime on the main sequence isproportional to its mass divided by its luminosity • The duration of a star’s main sequence lifetime depends on the amount of hydrogen in the star’s core and the rate at which the hydrogen is consumed• N.B. - The more massive a star, the shorter is its main-sequence lifetimeThe Sun has been a main-sequence star for about 4.56 billion years and should remain one for about another 7 billion yearsDuring a star’s main-sequence lifetime, the star expands somewhat and undergoes a modest increase in luminosityWhen core hydrogen fusion ceases, a main-sequence star becomes a red giantRed Giants• Core hydrogen fusion ceases when the hydrogen has been exhausted in the core of a main-sequence star• This leaves a core of nearly pure helium surrounded by a shell through which hydrogen fusion works its way outward in the star• The core shrinks and becomes hotter, while the star’s outer layers expand and cool• The result is a red giant starAs stars age and become giant stars,they expand tremendously and shed matter into space• When the central temperature of a red giant reaches about 100 million K, helium fusion begins in the core.• A process called the triple alpha process, converts helium to carbon and oxygen.• In a more massive red giant, helium fusion begins gradually• In a less massive red giant, it begins suddenly, in a process called the helium flashAfter the helium flash, a low-mass star moves quickly from the red-giant region of the H-R diagram to the horizontal branch• H-R diagrams and observations of star clustersreveal how red giants evolve• The age of a star cluster can be estimated by plotting its stars on an H-R diagramThe cluster’s age can be estimated by the age of the main-sequence stars at the turnoff point (the upper end of the remaining main sequence)As a cluster ages, the main sequence is “eaten away” from the upper left as stars of progressively smaller mass evolve into red giantsPopulations (generations) of stars• Relatively young Population I stars are metal rich; ancient Population II stars are metal poor• The metals (heavy elements) in Population I stars were manufactured by thermonuclear reactions in an earlier generation of Population II stars, then ejected into space and incorporated into a later stellar generationVariable StarsWhen a star’s evolutionary track carries it through a region in the H-R diagram called the instability strip, the star becomes unstable and begins to pulsate• Cepheid variables are high-mass variable stars• RR Lyrae variables are lower-mass, metal-poor variable stars with short periods• Long-period variable stars also pulsate but in a fashion that is less well understoodThere is a direct relationship between Cepheid periods of pulsation and their luminositiesMass transfer can affect the evolution of closebinary star systemsMass transfer in a close binary system occurs when one star in a close binary overflows its Roche lobeGas flowing from one star to the other passes across the inner Lagrangian pointThis mass transfer can affect the evolutionary history of the stars that make up the binary systemKey Words• alpha particle• Cepheid variable• close binary• color-magnitude diagram• contact binary• core helium fusion• core hydrogen fusion• degeneracy• degenerate-electron pressure• detached binary• globular cluster• helium flash• helium fusion• horizontal-branch star • ideal gas• inner Lagrangian point• instability strip• long-period variable• main-sequence lifetime• mass loss• mass transfer• metal-poor star• metal-rich star• overcontact binary• Pauli exclusion principle• period-luminosity relation• Population I and Population II stars• pulsating variable star• red giant• Roche lobe• RR Lyrae variable• semidetached binary• shell hydrogen fusion• triple alpha process• turnoff point• Type I and Type II Cepheids• zero-age main sequence (ZAMS)• zero-age main-sequence


View Full Document

MASON ASTR 113 - Stellar Evolution: After the Main Sequence

Download Stellar Evolution: After the Main Sequence
Our administrator received your request to download this document. We will send you the file to your email shortly.
Loading Unlocking...
Login

Join to view Stellar Evolution: After the Main Sequence and access 3M+ class-specific study document.

or
We will never post anything without your permission.
Don't have an account?
Sign Up

Join to view Stellar Evolution: After the Main Sequence 2 2 and access 3M+ class-specific study document.

or

By creating an account you agree to our Privacy Policy and Terms Of Use

Already a member?