Chapter 12 Stellar Evolution

12.1 Leaving the Main Sequence During its stay on the Main Sequence, any fluctuations in a star’s condition are quickly restored; the star is in equilibrium

12.1 Leaving the Main Sequence During its stay on the Main Sequence, any fluctuations in a star’s condition are quickly restored; the star is in equilibrium: A temperature increase in core increases fusion rate

12.1 Leaving the Main Sequence During its stay on the Main Sequence, any fluctuations in a star’s condition are quickly restored; the star is in equilibrium: A temperature increase in core increases fusion rate This increases pressure

12.1 Leaving the Main Sequence During its stay on the Main Sequence, any fluctuations in a star’s condition are quickly restored; the star is in equilibrium: A temperature increase in core increases fusion rate This increases pressure Star expands

12.1 Leaving the Main Sequence During its stay on the Main Sequence, any fluctuations in a star’s condition are quickly restored; the star is in equilibrium: A temperature increase in core increases fusion rate This increases pressure Star expands Expansion causes cooling

12.1 Leaving the Main Sequence During its stay on the Main Sequence, any fluctuations in a star’s condition are quickly restored; the star is in equilibrium: A temperature increase in core increases fusion rate This increases pressure Star expands Expansion causes cooling Fusion rate falls

12.1 Leaving the Main Sequence During its stay on the Main Sequence, any fluctuations in a star’s condition are quickly restored; the star is in equilibrium: A temperature increase in core increases fusion rate This increases pressure Star expands Expansion causes cooling Fusion rate falls Pressure decreases

12.1 Leaving the Main Sequence During its stay on the Main Sequence, any fluctuations in a star’s condition are quickly restored; the star is in equilibrium: A temperature increase in core increases fusion rate This increases pressure Star expands Expansion causes cooling Fusion rate falls Pressure decreases Star returns to original size

12.1 Leaving the Main Sequence During its stay on the Main Sequence, any fluctuations in a star’s condition are quickly restored; the star is in equilibrium: A temperature increase in core increases fusion rate This increases pressure Star expands Expansion causes cooling Fusion rate falls Pressure decreases Star returns to original size A temperature decrease causes the opposite

12.1 Leaving the Main Sequence Eventually, as hydrogen in the core is consumed, the star begins to leave the Main Sequence. Its evolution from then on depends very much on the mass of the star: Low-mass stars go quietly High-mass stars go out with a bang!

12.2 Evolution of a Sun-like Star Even while on the Main Sequence, the composition of a star’s core is changing:

12.2 Evolution of a Sun-like Star Even while on the Main Sequence, the composition of a star’s core is changing:

12.2 Evolution of a Sun-like Star Even while on the Main Sequence, the composition of a star’s core is changing:

12.2 Evolution of a Sun-like Star Even while on the Main Sequence, the composition of a star’s core is changing: As the fuel in the core is used up, the core contracts

12.2 Evolution of a Sun-like Star When the fuel in the core is used up, the core begins to collapse.

12.2 Evolution of a Sun-like Star When the fuel in the core is used up, the core begins to collapse. The collapsing core heats up

12.2 Evolution of a Sun-like Star When the fuel in the core is used up, the core begins to collapse. The collapsing core heats up Hydrogen begins to fuse outside the core

12.2 Evolution of a Sun-like Star When the fuel in the core is used up, the core begins to collapse. The collapsing core heats up Hydrogen begins to fuse outside the core The fusion rate is even higher than on the main sequence

12.2 Evolution of a Sun-like Star When the fuel in the core is used up, the core begins to collapse. The collapsing core heats up Hydrogen begins to fuse outside the core The fusion rate is even higher than on the main sequence The star is on its way to becoming a red giant

12.2 Evolution of a Sun-like Star Stages of a star leaving the Main Sequence:

12.2 Evolution of a Sun-like Star Stage 9: The Red-Giant Branch As the core continues to shrink, the outer layers of the star expand and cool.

12.2 Evolution of a Sun-like Star Stage 9: The Red-Giant Branch As the core continues to shrink, the outer layers of the star expand and cool. It is now a red giant, extending out as far as the orbit of Mercury.

12.2 Evolution of a Sun-like Star Stage 9: The Red-Giant Branch As the core continues to shrink, the outer layers of the star expand and cool. It is now a red giant, extending out as far as the orbit of Mercury. Despite its cooler temperature, its luminosity increases enormously due to its large size.

12.2 Evolution of a Sun-like Star Stage 9: The Red-Giant Branch As the core continues to shrink, the outer layers of the star expand and cool. It is now a red giant, extending out as far as the orbit of Mercury. Despite its cooler temperature, its luminosity increases enormously due to its large size. The increased luminosity comes from the increased fusion rate.

12.2 Evolution of a Sun-like Star The red giant stage on the H-R diagram:

12.2 Evolution of a Sun-like Star Stage 10: Helium fusion Once the core temperature has risen to 100,000,000 K, the helium in the core starts to fuse at the helium flash

12.2 Evolution of a Sun-like Star Stage 10: Helium fusion Once the core temperature has risen to 100,000,000 K, the helium in the core starts to fuse at the helium flash Helium begins to fuse extremely rapidly

12.2 Evolution of a Sun-like Star Stage 10: Helium fusion Once the core temperature has risen to 100,000,000 K, the helium in the core starts to fuse at the helium flash Helium begins to fuse extremely rapidly Within hours the enormous energy output is over, and the star once again reaches equilibrium

12.2 Evolution of a Sun-like Star Stage 10 on the H-R diagram:

12.2 Evolution of a Sun-like Star Stage 11: Back to the giant branch As the helium in the core fuses to carbon, the core becomes hotter and hotter, and the helium burns faster and faster. The star is now similar to its condition just as it left the Main Sequence, except now there are two shells:

12.2 Evolution of a Sun-like Star The star has become a red giant for the second time:

12.3 The Death of a Low-Mass Star This graphic shows the entire evolution of a Sun-like star. Such stars never become hot enough (600,000,000 K) for carbon fusion to take place. This is because electron degeneracy pressure stops the collapse of the carbon core.

12.3 The Death of a Low-Mass Star The carbon core, with no outward fusion pressure, continues to contract until the degeneracy pressure point is reached Meanwhile, the outer layers of the star expand to form a planetary nebula.

12.3 The Death of a Low-Mass Star The star now has two parts: A small, extremely dense carbon core An envelope about the size of our solar system. The envelope is called a planetary nebula, even though it has nothing to do with planets – early astronomers viewing the fuzzy envelope thought it resembled a planetary system.

12.3 The Death of a Low-Mass Star Stages 13 and 14: White and black dwarfs Once the nebula has gone, the remaining core is extremely dense and extremely hot, but quite small. It is luminous only due to its high temperature.

12.3 The Death of a Low-Mass Star The small star Sirius B is a white-dwarf companion of the much larger and brighter Sirius A:

12.3 The Death of a Low-Mass Star The Hubble Space Telescope has detected white dwarf stars (circled) in globular clusters:

12.3 The Death of a Low-Mass Star As the white dwarf cools, its size does not change significantly; it simply gets dimmer and dimmer, and finally ceases to glow.

12.3 The Death of a Low-Mass Star A nova is a star that flares up very suddenly and then returns slowly to its former luminosity:

12.3 The Death of a Low-Mass Star A white dwarf that is part of a close binary system can undergo repeated novas:

12.3 The Death of a Low-Mass Star Material falls onto the white dwarf from its main-sequence companion. When enough material has accreted, fusion can reignite very suddenly, burning off the new material. Material keeps being transferred to the white dwarf, and the process repeats.

End of 16 April 2007 Lecture

12.3 The Death of a Low-Mass Star This graphic shows the entire evolution of a Sun-like star. Such stars never become hot enough (600,000,000 K) for carbon fusion to take place. This is because electron degeneracy pressure stops the collapse of the carbon core.

12.3 The Death of a Low-Mass Star Stages 13 and 14: White and black dwarfs Once the nebula has gone, the remaining core is extremely dense and extremely hot, but quite small. It is luminous only due to its high temperature.

12.4 Evolution of Stars More Massive than the Sun It can be seen from this H-R diagram that stars more massive than the Sun follow very different paths when leaving the Main Sequence:

12.4 Evolution of Stars More Massive than the Sun High-mass stars, like all stars, leave the Main Sequence when there is no more hydrogen fuel in their cores.

12.4 Evolution of Stars More Massive than the Sun High-mass stars, like all stars, leave the Main Sequence when there is no more hydrogen fuel in their cores. The first few events are similar to those in lower-mass stars – first a hydrogen shell, then a core burning helium to carbon, surrounded by helium- and hydrogen-burning shells.

12.4 Evolution of Stars More Massive than the Sun A star of more than 8 solar masses can fuse elements far beyond carbon in its core, leading to a very different fate. Eventually the star dies in a violent explosion called a supernova.

12.4 Evolution of Stars More Massive than the Sun A star of more than 8 solar masses can fuse elements far beyond carbon in its core, leading to a very different fate. Eventually the star dies in a violent explosion called a supernova. This happens when the fusion product is iron

12.4 Evolution of Stars More Massive than the Sun The “ashes” of earlier fusion reactions start fusing

12.4 Evolution of Stars More Massive than the Sun The “ashes” of earlier fusion reactions start fusing Core looks like onion

12.4 Evolution of Stars More Massive than the Sun The “ashes” of earlier fusion reactions start fusing Core looks like onion Finally, iron is produced

12.4 Evolution of Stars More Massive than the Sun The “ashes” of earlier fusion reactions start fusing Core looks like onion Finally, iron is produced Iron can’t fuse

12.4 Evolution of Stars More Massive than the Sun The “ashes” of earlier fusion reactions start fusing Core looks like onion Finally, iron is produced Iron can’t fuse Iron core collapses

12.4 Evolution of Stars More Massive than the Sun The “ashes” of earlier fusion reactions start fusing Core looks like onion Finally, iron is produced Iron can’t fuse Iron core collapses SUPERNOVA

12.4 Evolution of Stars More Massive than the Sun

12.4 Evolution of Stars More Massive than the Sun But just said >8!

12.4 Evolution of Stars More Massive than the Sun But just said >8!

12.5 Supernova Explosions A supernova is a one-time event – once it happens, there is little or nothing left of the progenitor star.

12.5 Supernova Explosions A supernova is a one-time event – once it happens, there is little or nothing left of the progenitor star. There are two different types of supernovae, both equally common:

12.5 Supernova Explosions A supernova is a one-time event – once it happens, there is little or nothing left of the progenitor star. There are two different types of supernovae, both equally common: Type II, which is the death of a high-mass star we already discussed

12.5 Supernova Explosions A supernova is a one-time event – once it happens, there is little or nothing left of the progenitor star. There are two different types of supernovae, both equally common: Type II, which is the death of a high-mass star we already discussed Type I, which is a carbon-detonation supernova

12.5 Supernova Explosions Carbon-detonation supernova occurs when a white dwarf has accumulated too much mass from a binary companion

12.5 Supernova Explosions Carbon-detonation supernova occurs when a white dwarf has accumulated too much mass from a binary companion…novas can occur beforehand

12.5 Supernova Explosions Carbon-detonation supernova occurs when a white dwarf has accumulated too much mass from a binary companion…novas can occur beforehand If the white dwarf’s mass exceeds 1.4 solar masses, electron degeneracy can no longer keep the core from collapsing.

12.5 Supernova Explosions Carbon-detonation supernova occurs when a white dwarf has accumulated too much mass from a binary companion…novas can occur beforehand If the white dwarf’s mass exceeds 1.4 solar masses, electron degeneracy can no longer keep the core from collapsing. Carbon fusion begins throughout the star almost simultaneously, resulting in a carbon explosion.

12.5 Supernova Explosions This graphic illustrates the two different types of supernovae:

12.5 Supernova Explosions The two types – each of which is more than a million times as bright as a nova – can be distinguished by their light curves and their spectra

12.5 Supernova Explosions Supernovae leave remnants – the expanding clouds of material from the explosion. The Crab nebula is a remnant from a supernova explosion that occurred in the year 1054.

12.6 Observing Stellar Evolution in Star Clusters The following series of H-R diagrams shows how stars of the same age, but different masses, appear as the cluster as a whole ages. After 10 million years, the most massive stars have already left the Main Sequence, while many of the least massive have not even reached it yet.

12.6 Observing Stellar Evolution in Star Clusters After 100 million years, a distinct main-sequence turnoff begins to develop. This shows the highest-mass stars that are still on the Main Sequence. After 1 billion years, the main-sequence turnoff is much clearer.

12.6 Observing Stellar Evolution in Star Clusters After 10 billion years, a number of features are evident: The red-giant, subgiant, asymptotic giant, and horizontal branches are all clearly populated. White dwarfs, indicating that solar-mass stars are in their last phases, also appear.

12.6 Observing Stellar Evolution in Star Clusters This double cluster, h and chi Persei, must be quite young – its H-R diagram is that of a newborn cluster. Its age cannot be more than about 10 million years.

12.6 Observing Stellar Evolution in Star Clusters The Hyades cluster, shown here, is also rather young; its main-sequence turnoff indicates an age of about 600 million years.

12.6 Observing Stellar Evolution in Star Clusters This globular cluster, M80, is about 10-12 billion years old, much older than the previous examples.

12.7 The Cycle of Stellar Evolution Star formation is cyclical: stars form, evolve, and die. In dying, they send heavy elements into the interstellar medium. These elements then become parts of new stars. And so it goes.

Summary of Chapter 12 Once hydrogen is gone in the core, a star burns hydrogen in the surrounding shell. The core contracts and heats; the outer atmosphere expands and cools. Helium begins to fuse in the core, as a helium flash. The star expands into a red giant as the core continues to collapse. The envelope blows off, leaving a white dwarf to gradually cool. Nova results from material accreting onto a white dwarf from a companion star

Summary of Chapter 12 Massive stars become hot enough to fuse carbon, then heavier elements all the way to iron. At the end, the core collapses and rebounds as a Type II supernova. Type I supernova is a carbon explosion, occurring when too much mass falls onto a white dwarf. All heavy elements are formed in stellar cores or in supernovae. Stellar evolution can be understood by observing star clusters.